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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Hammache%2C+F&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Hammache%2C+F&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Hammache%2C+F&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.09480">arXiv:2411.09480</a> <span> [<a href="https://arxiv.org/pdf/2411.09480">pdf</a>, <a href="https://arxiv.org/format/2411.09480">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.110.024610">10.1103/PhysRevC.110.024610 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mirror nucleon-transfer reactions from $^{18}$Ne and $^{18}$O </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Keeley%2C+N">N. Keeley</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillibert%2C+A">A. Gillibert</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Audirac%2C+L">L. Audirac</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Boissinot%2C+S">S. Boissinot</a>, <a href="/search/nucl-ex?searchtype=author&query=Caccitti%2C+J">J. Caccitti</a>, <a href="/search/nucl-ex?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/nucl-ex?searchtype=author&query=Damoy%2C+S">S. Damoy</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gangnant%2C+P">P. Gangnant</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Goupil%2C+J">J. Goupil</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Houarner%2C+C">C. Houarner</a>, <a href="/search/nucl-ex?searchtype=author&query=Jacquot%2C+B">B. Jacquot</a>, <a href="/search/nucl-ex?searchtype=author&query=Lebertre%2C+G">G. Lebertre</a>, <a href="/search/nucl-ex?searchtype=author&query=Legeard%2C+L">L. Legeard</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%A9nager%2C+L">L. M茅nager</a>, <a href="/search/nucl-ex?searchtype=author&query=Morel%2C+V">V. Morel</a>, <a href="/search/nucl-ex?searchtype=author&query=Morfouace%2C+P">P. Morfouace</a>, <a href="/search/nucl-ex?searchtype=author&query=Pancin%2C+J">J. Pancin</a>, <a href="/search/nucl-ex?searchtype=author&query=Pollacco%2C+E+C">E. C. Pollacco</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.09480v1-abstract-short" style="display: inline;"> The $^{18}$Ne(d,t)$^{17}$Ne and $^{18}$Ne(d,$^3$He)$^{17}$F single-nucleon pickup reactions were measured at 16.5 MeV/nucleon in inverse kinematics together with elastic and inelastic scattering channels. The full set of measured exclusive differential cross sections was compared with the mirror reaction channels on stable $^{18}$O after consistent reanalysis using coupled reaction channels calcul… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09480v1-abstract-full').style.display = 'inline'; document.getElementById('2411.09480v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09480v1-abstract-full" style="display: none;"> The $^{18}$Ne(d,t)$^{17}$Ne and $^{18}$Ne(d,$^3$He)$^{17}$F single-nucleon pickup reactions were measured at 16.5 MeV/nucleon in inverse kinematics together with elastic and inelastic scattering channels. The full set of measured exclusive differential cross sections was compared with the mirror reaction channels on stable $^{18}$O after consistent reanalysis using coupled reaction channels calculations. Within this interpretation scheme, most of the spectroscopic factors extracted for the population of unbound states in $^{17}$F match within uncertainties with their mirror partners in $^{17}$O. However, for the deeply-bound neutron removal channel to $^{17}$Ne, a significant symmetry breaking with the mirror proton-removal channel leading to $^{17}$N is evidenced by an overall single-particle strength reduction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09480v1-abstract-full').style.display = 'none'; document.getElementById('2411.09480v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 110, 024610 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.12594">arXiv:2409.12594</a> <span> [<a href="https://arxiv.org/pdf/2409.12594">pdf</a>, <a href="https://arxiv.org/format/2409.12594">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Probing exotic cross-shell interactions at N=28 with single-neutron transfer on 47K </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Paxman%2C+C+J">C. J. Paxman</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W+N">W. N. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Lotay%2C+G">G. Lotay</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Ramos%2C+D">D. Ramos</a>, <a href="/search/nucl-ex?searchtype=author&query=Orr%2C+N+A">N. A. Orr</a>, <a href="/search/nucl-ex?searchtype=author&query=Galtarossa%2C+F">F. Galtarossa</a>, <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Dudouet%2C+J">J. Dudouet</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+N+L">N. L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Ackermann%2C+D">D. Ackermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrientos%2C+D">D. Barrientos</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Bednarczyk%2C+P">P. Bednarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Benzoni%2C+G">G. Benzoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Bracco%2C+A">A. Bracco</a>, <a href="/search/nucl-ex?searchtype=author&query=Canete%2C+L">L. Canete</a>, <a href="/search/nucl-ex?searchtype=author&query=Cederwall%2C+B">B. Cederwall</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciemala%2C+M">M. Ciemala</a>, <a href="/search/nucl-ex?searchtype=author&query=Delahaye%2C+P">P. Delahaye</a>, <a href="/search/nucl-ex?searchtype=author&query=Doherty%2C+D+T">D. T. Doherty</a>, <a href="/search/nucl-ex?searchtype=author&query=Domingo-Pardo%2C+C">C. Domingo-Pardo</a> , et al. (54 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.12594v1-abstract-short" style="display: inline;"> We present the first measurement of the $^{47}$K($d,p纬$)$^{48}$K transfer reaction, performed in inverse kinematics using a reaccelerated beam of $^{47}$K. The level scheme of $^{48}$K has been greatly extended with nine new bound excited states identified and spectroscopic factors deduced. Detailed comparisons with SDPF-U and SDPF-MU shell-model calculations reveal a number of discrepancies with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12594v1-abstract-full').style.display = 'inline'; document.getElementById('2409.12594v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.12594v1-abstract-full" style="display: none;"> We present the first measurement of the $^{47}$K($d,p纬$)$^{48}$K transfer reaction, performed in inverse kinematics using a reaccelerated beam of $^{47}$K. The level scheme of $^{48}$K has been greatly extended with nine new bound excited states identified and spectroscopic factors deduced. Detailed comparisons with SDPF-U and SDPF-MU shell-model calculations reveal a number of discrepancies with these results, and a preference for SDPF-MU is found. Intriguingly, an apparent systematic overestimation of spectroscopic factors and a poor reproduction of the energies for 1$^-$ states suggests that the mixing between the $蟺s^{\,\,\,1}_{1/2} d^{\,\,\,4}_{3/2}$ and $蟺s^{\,\,\,2}_{1/2} d^{\,\,\,3}_{3/2}$ proton configurations in $^{48}$K is not correctly described using current interactions, challenging our descriptions of light $N=28$ nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.12594v1-abstract-full').style.display = 'none'; document.getElementById('2409.12594v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14305">arXiv:2405.14305</a> <span> [<a href="https://arxiv.org/pdf/2405.14305">pdf</a>, <a href="https://arxiv.org/format/2405.14305">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.131.262501">10.1103/PhysRevLett.131.262501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-precision spectroscopy of $^{20}$O benchmarking ab-initio calculations in light nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Zanon%2C+I">I. Zanon</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Goasduff%2C+A">A. Goasduff</a>, <a href="/search/nucl-ex?searchtype=author&query=Men%C3%A9ndez%2C+J">J. Men茅ndez</a>, <a href="/search/nucl-ex?searchtype=author&query=Miyagi%2C+T">T. Miyagi</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciema%C5%82a%2C+M">M. Ciema艂a</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Ramos%2C+D">D. Ramos</a>, <a href="/search/nucl-ex?searchtype=author&query=Rejmund%2C+M">M. Rejmund</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+L">L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Ackermann%2C+D">D. Ackermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrientos%2C+D">D. Barrientos</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Benzoni%2C+G">G. Benzoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Boston%2C+A+J">A. J. Boston</a>, <a href="/search/nucl-ex?searchtype=author&query=Boston%2C+H+C">H. C. Boston</a>, <a href="/search/nucl-ex?searchtype=author&query=Bottoni%2C+S">S. Bottoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Bracco%2C+A">A. Bracco</a>, <a href="/search/nucl-ex?searchtype=author&query=Brugnara%2C+D">D. Brugnara</a>, <a href="/search/nucl-ex?searchtype=author&query=de+France%2C+G">G. de France</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Sereville%2C+N">N. de Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a> , et al. (56 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.14305v1-abstract-short" style="display: inline;"> The excited states of unstable $^{20}$O were investigated via $纬$-ray spectroscopy following the $^{19}$O$(d,p)^{20}$O reaction at 8 $A$MeV. By exploiting the Doppler Shift Attenuation Method, the lifetime of the 2$^+_2$ and 3$^+_1$ states were firmly established. From the $纬$-ray branching and E2/M1 mixing ratios for transitions deexciting the 2$^+_2$ and 3$^+_1$ states, the B(E2) and B(M1) were… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14305v1-abstract-full').style.display = 'inline'; document.getElementById('2405.14305v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14305v1-abstract-full" style="display: none;"> The excited states of unstable $^{20}$O were investigated via $纬$-ray spectroscopy following the $^{19}$O$(d,p)^{20}$O reaction at 8 $A$MeV. By exploiting the Doppler Shift Attenuation Method, the lifetime of the 2$^+_2$ and 3$^+_1$ states were firmly established. From the $纬$-ray branching and E2/M1 mixing ratios for transitions deexciting the 2$^+_2$ and 3$^+_1$ states, the B(E2) and B(M1) were determined. Various chiral effective field theory Hamiltonians, describing the nuclear properties beyond ground states, along with a standard USDB interaction, were compared with the experimentally obtained data. Such a comparison for a large set of $纬$-ray transition probabilities with the valence space in medium similarity renormalization group ab-initio calculations was performed for the first time in a nucleus far from stability. It was shown that the ab-initio approaches using chiral EFT forces are challenged by detailed high-precision spectroscopic properties of nuclei. The reduced transition probabilities were found to be a very constraining test of the performance of the ab-initio models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14305v1-abstract-full').style.display = 'none'; document.getElementById('2405.14305v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Supplemental Material available</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physical Review Letter 131, 262501 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13129">arXiv:2311.13129</a> <span> [<a href="https://arxiv.org/pdf/2311.13129">pdf</a>, <a href="https://arxiv.org/format/2311.13129">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.131.212501">10.1103/PhysRevLett.131.212501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Validation of the $^{10}\mathrm{Be}$ Ground-State Molecular Structure Using $^{10}\mathrm{Be}(p,p伪)^{6}\mathrm{He}$ Triple Differential Reaction Cross-Section Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Li%2C+P+J">P. J. Li</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Harada%2C+T">T. Harada</a>, <a href="/search/nucl-ex?searchtype=author&query=Kanada-En%27yo%2C+Y">Y. Kanada-En'yo</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubota%2C+Y">Y. Kubota</a>, <a href="/search/nucl-ex?searchtype=author&query=Leblond%2C+S">S. Leblond</a>, <a href="/search/nucl-ex?searchtype=author&query=Liang%2C+P+F">P. F. Liang</a>, <a href="/search/nucl-ex?searchtype=author&query=Lokotko%2C+T">T. Lokotko</a>, <a href="/search/nucl-ex?searchtype=author&query=Lyu%2C+M">M. Lyu</a>, <a href="/search/nucl-ex?searchtype=author&query=Marqu%C3%A9s%2C+F+M">F. M. Marqu茅s</a>, <a href="/search/nucl-ex?searchtype=author&query=Matsuda%2C+Y">Y. Matsuda</a>, <a href="/search/nucl-ex?searchtype=author&query=Ogata%2C+K">K. Ogata</a>, <a href="/search/nucl-ex?searchtype=author&query=Otsu%2C+H">H. Otsu</a>, <a href="/search/nucl-ex?searchtype=author&query=Rindel%2C+E">E. Rindel</a>, <a href="/search/nucl-ex?searchtype=author&query=Stuhl%2C+L">L. Stuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Togano%2C+Y">Y. Togano</a>, <a href="/search/nucl-ex?searchtype=author&query=Tomai%2C+T">T. Tomai</a>, <a href="/search/nucl-ex?searchtype=author&query=Xu%2C+X+X">X. X. Xu</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.13129v1-abstract-short" style="display: inline;"> The cluster structure of the neutron-rich isotope $^{10}$Be has been probed via the $(p,p伪)$ reaction at 150 MeV/nucleon in inverse kinematics and in quasifree conditions. The populated states of $^{6}$He residues were investigated through missing mass spectroscopy. The triple differential cross-section for the ground-state transition was extracted for quasifree angle pairs ($胃_{p}$, $胃_伪$) and co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13129v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13129v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13129v1-abstract-full" style="display: none;"> The cluster structure of the neutron-rich isotope $^{10}$Be has been probed via the $(p,p伪)$ reaction at 150 MeV/nucleon in inverse kinematics and in quasifree conditions. The populated states of $^{6}$He residues were investigated through missing mass spectroscopy. The triple differential cross-section for the ground-state transition was extracted for quasifree angle pairs ($胃_{p}$, $胃_伪$) and compared to distorted-wave impulse approximation reaction calculations performed in a microscopic framework using successively the Tohsaki-Horiuchi-Schuck-R枚pke product wave-function and the wave-function deduced from Antisymmetrized Molecular Dynamics calculations. The remarkable agreement between calculated and measured cross-sections in both shape and magnitude validates the molecular structure description of the $^{10}$Be ground-state, configured as an $伪$-$伪$ core with two valence neutrons occupying $蟺$-type molecular orbitals. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13129v1-abstract-full').style.display = 'none'; document.getElementById('2311.13129v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, 1 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 131 (2023) 212501 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.14382">arXiv:2302.14382</a> <span> [<a href="https://arxiv.org/pdf/2302.14382">pdf</a>, <a href="https://arxiv.org/format/2302.14382">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> N=16 magicity revealed at the proton drip-line through the study of 35Ca </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Lalanne%2C+L">L. Lalanne</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Poves%2C+A">A. Poves</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Koyama%2C+S">S. Koyama</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Roger%2C+T">T. Roger</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+D+O">F. De Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Kamalou%2C+O">O. Kamalou</a>, <a href="/search/nucl-ex?searchtype=author&query=Kitamura%2C+N">N. Kitamura</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Mauss%2C+B">B. Mauss</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.14382v1-abstract-short" style="display: inline;"> The last proton bound calcium isotope $^{35}$Ca has been studied for the first time, using the $^{37}$Ca($p, t$)$^{35}$Ca two neutron transfer reaction. The radioactive $^{37}$Ca nuclei, produced by the LISE spectrometer at GANIL, interacted with the protons of the liquid hydrogen target CRYPTA, to produce tritons $t$ that were detected in the MUST2 detector array, in coincidence with the heavy re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14382v1-abstract-full').style.display = 'inline'; document.getElementById('2302.14382v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14382v1-abstract-full" style="display: none;"> The last proton bound calcium isotope $^{35}$Ca has been studied for the first time, using the $^{37}$Ca($p, t$)$^{35}$Ca two neutron transfer reaction. The radioactive $^{37}$Ca nuclei, produced by the LISE spectrometer at GANIL, interacted with the protons of the liquid hydrogen target CRYPTA, to produce tritons $t$ that were detected in the MUST2 detector array, in coincidence with the heavy residues Ca or Ar. The atomic mass of $^{35}$Ca and the energy of its first 3/2$^+$ state are reported. A large $N=16$ gap of 4.61(11) MeV is deduced from the mass measurement, which together with other measured properties, makes $^{36}$Ca a doubly-magic nucleus. The $N = 16$ shell gaps in $^{36}$Ca and $^{24}$O are of similar amplitude, at both edges of the valley of stability. This feature is discussed in terms of nuclear forces involved, within state-of-the-art shell model calculations. Even though the global agreement with data is quite convincing, the calculations underestimate the size of the $N = 16$ gap in 36Ca by 840(110) keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14382v1-abstract-full').style.display = 'none'; document.getElementById('2302.14382v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.12939">arXiv:2302.12939</a> <span> [<a href="https://arxiv.org/pdf/2302.12939">pdf</a>, <a href="https://arxiv.org/format/2302.12939">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.108.045802">10.1103/PhysRevC.108.045802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for resonance states in $^{22}$Ne($p,纬$)$^{23}$Na </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Carrasco-Rojas%2C+D+P">D. P. Carrasco-Rojas</a>, <a href="/search/nucl-ex?searchtype=author&query=Williams%2C+M">M. Williams</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L. Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Fougeres%2C+C">C. Fougeres</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Harrouz%2C+D+S">D. S. Harrouz</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Palmerini%2C+S">S. Palmerini</a>, <a href="/search/nucl-ex?searchtype=author&query=Pizzone%2C+R+G">R. G. Pizzone</a>, <a href="/search/nucl-ex?searchtype=author&query=Romano%2C+S">S. Romano</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Sereville%2C+N">N. de Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Tumino%2C+A">A. Tumino</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.12939v2-abstract-short" style="display: inline;"> Background: Globular clusters show strong correlations between different elements, such as the well-known sodium-oxygen anticorrelation. One of the main sources of uncertainty in this anticorrelation is the $^{22}$Ne($p,纬$)$^{23}$Na reaction rate, due to the possible influence of an unobserved resonance state at $E_\mathrm{x} = 8862$ keV ($E_\mathrm{r, c.m.} = 68$ keV). The influence of two higher… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.12939v2-abstract-full').style.display = 'inline'; document.getElementById('2302.12939v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.12939v2-abstract-full" style="display: none;"> Background: Globular clusters show strong correlations between different elements, such as the well-known sodium-oxygen anticorrelation. One of the main sources of uncertainty in this anticorrelation is the $^{22}$Ne($p,纬$)$^{23}$Na reaction rate, due to the possible influence of an unobserved resonance state at $E_\mathrm{x} = 8862$ keV ($E_\mathrm{r, c.m.} = 68$ keV). The influence of two higher-lying resonance states at $E_\mathrm{x} = 8894$ and $9000$ keV has already been ruled out by direct $^{22}$Ne($p,纬$)$^{23}$Na measurementsPurpose: To study excited states in $^{23}$Na above the proton threshold to determine if the unconfirmed resonance states in $^{23}$Na exist. Methods: The non-selective proton inelastic scattering reaction at low energies was used to search for excited states in $^{23}$Na above the proton threshold. Protons scattered from various targets were momentum-analysed in the Q3D magnetic spectrograph at the Maier-Leibnitz Laboratorium, Munich, Germany. Results: The resonance states previously reported at $E_\mathrm{x} = 8862$, $8894$ and $9000$ keV in other experiments were not observed in the present experiment at any angle. This result, combined with other non-observations of these resonance states in most other experiments, results in a strong presumption against the existence of these resonance states. Conclusions: The previously reported resonance states at $E_\mathrm{x} = 8862$, $8894$ and $9000$ keV are unlikely to exist and should be omitted from future evaluations of the $^{22}$Ne($p,纬$)$^{23}$Na reaction rates. Indirect studies using low-energy proton inelastic scattering are a simple and yet exceptionally powerful tool in helping to constrain astrophysical reaction rates by providing non-selective information of the excited states of nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.12939v2-abstract-full').style.display = 'none'; document.getElementById('2302.12939v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">1 single-panel figure and 5 double-panel figures. Updated version of paper with better organisation of parts</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.08382">arXiv:2302.08382</a> <span> [<a href="https://arxiv.org/pdf/2302.08382">pdf</a>, <a href="https://arxiv.org/format/2302.08382">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> Cross-shell states in $^{15}$C: a test for p-sd interactions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Lois-Fuentes%2C+J">J. Lois-Fuentes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fern%C3%A1ndez-Dom%C3%ADnguez%2C+B">B. Fern谩ndez-Dom铆nguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Pereira-L%C3%B3pez%2C+X">X. Pereira-L贸pez</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W+N">W. N. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Orr%2C+N+A">N. A. Orr</a>, <a href="/search/nucl-ex?searchtype=author&query=Duguet%2C+T">T. Duguet</a>, <a href="/search/nucl-ex?searchtype=author&query=Otsuka%2C+T">T. Otsuka</a>, <a href="/search/nucl-ex?searchtype=author&query=Som%C3%A0%2C+V">V. Som脿</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+N+L">N. L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y. Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Caama%C3%B1o%2C+M">M. Caama帽o</a>, <a href="/search/nucl-ex?searchtype=author&query=Caceres%2C+L">L. Caceres</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/nucl-ex?searchtype=author&query=Curtis%2C+N">N. Curtis</a>, <a href="/search/nucl-ex?searchtype=author&query=Deshayes%2C+Q">Q. Deshayes</a>, <a href="/search/nucl-ex?searchtype=author&query=Farget%2C+F">F. Farget</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.08382v1-abstract-short" style="display: inline;"> The low-lying structure of $^{15}$C has been investigated via the neutron-removal $^{16}$C$(d,t)$ reaction. Along with bound neutron sd-shell hole states, unbound p-shell hole states have been firmly confirmed. The excitation energies and the deduced spectroscopic factors of the cross-shell states are an important measure of the $[(p)^{-1}(sd)^{2}]$ neutron configurations in $^{15}$C. Our results… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08382v1-abstract-full').style.display = 'inline'; document.getElementById('2302.08382v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.08382v1-abstract-full" style="display: none;"> The low-lying structure of $^{15}$C has been investigated via the neutron-removal $^{16}$C$(d,t)$ reaction. Along with bound neutron sd-shell hole states, unbound p-shell hole states have been firmly confirmed. The excitation energies and the deduced spectroscopic factors of the cross-shell states are an important measure of the $[(p)^{-1}(sd)^{2}]$ neutron configurations in $^{15}$C. Our results show a very good agreement with shell-model calculations using the SFO-tls interaction for $^{15}$C. However, a modification of the $p$-$sd$ and $sd$-$sd$ monopole terms was applied in order to reproduce the $N=9$ isotone $^{17}$O. In addition, the excitation energies and spectroscopic factors have been compared to the first calculations of $^{15}$C with the $ab~ initio$ self-consistent Green's function method employing the NNLO$_{sat}$ interaction. The results show the sensitivity to the size of the $N=8$ shell gap and highlight the need of going beyond the current truncation scheme in the theory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.08382v1-abstract-full').style.display = 'none'; document.getElementById('2302.08382v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.03648">arXiv:2212.03648</a> <span> [<a href="https://arxiv.org/pdf/2212.03648">pdf</a>, <a href="https://arxiv.org/format/2212.03648">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> Understanding globular cluster abundances through nuclear reactions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Williams%2C+M">M Williams</a>, <a href="/search/nucl-ex?searchtype=author&query=Harrouz%2C+D+S">D S Harrouz</a>, <a href="/search/nucl-ex?searchtype=author&query=Carrasco-Rojas%2C+D+P">D P Carrasco-Rojas</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Davids%2C+B">B Davids</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Foug%C3%A8res%2C+C">C Foug猫res</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hutcheon%2C+D">D Hutcheon</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A">AM Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Lennarz%2C+A">A Lennarz</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d">F d'Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Palmerini%2C+S">S Palmerini</a>, <a href="/search/nucl-ex?searchtype=author&query=Psaltis%2C+A">A Psaltis</a>, <a href="/search/nucl-ex?searchtype=author&query=Pizzone%2C+R+G">R G Pizzone</a>, <a href="/search/nucl-ex?searchtype=author&query=Romano%2C+S">S Romano</a>, <a href="/search/nucl-ex?searchtype=author&query=Ruiz%2C+C">C Ruiz</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.03648v1-abstract-short" style="display: inline;"> Globular clusters contain multiple stellar populations, with some previous generation of stars polluting the current stars with heavier elements. Understanding the history of globular clusters is helpful in understanding how galaxies merged and evolved and therefore constraining the site or sites of this historic pollution is a priority. The acceptable temperature and density conditions of these p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03648v1-abstract-full').style.display = 'inline'; document.getElementById('2212.03648v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.03648v1-abstract-full" style="display: none;"> Globular clusters contain multiple stellar populations, with some previous generation of stars polluting the current stars with heavier elements. Understanding the history of globular clusters is helpful in understanding how galaxies merged and evolved and therefore constraining the site or sites of this historic pollution is a priority. The acceptable temperature and density conditions of these polluting sites depend on critical reaction rates. In this paper, three experimental studies helping to constrain astrophysically important reaction rates are briefly discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.03648v1-abstract-full').style.display = 'none'; document.getElementById('2212.03648v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submission to conference proceedings of INPC2022 in Cape Town</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.11724">arXiv:2204.11724</a> <span> [<a href="https://arxiv.org/pdf/2204.11724">pdf</a>, <a href="https://arxiv.org/ps/2204.11724">ps</a>, <a href="https://arxiv.org/format/2204.11724">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nuclphysa.2023.122622">10.1016/j.nuclphysa.2023.122622 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gamma-ray emission in proton-induced nuclear reactions on natC and Mylar targets over the incident energy range of Ep = 30-200 MeV. Astrophysical implications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Rahma%2C+Y">Y. Rahma</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+E+A">E. A. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+J+J">J. J. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Belhout%2C+A">A. Belhout</a>, <a href="/search/nucl-ex?searchtype=author&query=Moussa%2C+D">D. Moussa</a>, <a href="/search/nucl-ex?searchtype=author&query=Yahia-Cherif%2C+W">W. Yahia-Cherif</a>, <a href="/search/nucl-ex?searchtype=author&query=Benhabiles-Mezhoud%2C+H">H. Benhabiles-Mezhoud</a>, <a href="/search/nucl-ex?searchtype=author&query=Bucher%2C+T+D">T. D. Bucher</a>, <a href="/search/nucl-ex?searchtype=author&query=Dinoko%2C+T+R+S">T. R. S. Dinoko</a>, <a href="/search/nucl-ex?searchtype=author&query=Chafa%2C+A">A. Chafa</a>, <a href="/search/nucl-ex?searchtype=author&query=Conradie%2C+J+L">J. L. Conradie</a>, <a href="/search/nucl-ex?searchtype=author&query=Damache%2C+S">S. Damache</a>, <a href="/search/nucl-ex?searchtype=author&query=Debabi%2C+M">M. Debabi</a>, <a href="/search/nucl-ex?searchtype=author&query=Deloncle%2C+I">I. Deloncle</a>, <a href="/search/nucl-ex?searchtype=author&query=Easton%2C+J+L">J. L. Easton</a>, <a href="/search/nucl-ex?searchtype=author&query=Fouka%2C+M">M. Fouka</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Jones%2C+P">P. Jones</a>, <a href="/search/nucl-ex?searchtype=author&query=Kheswa%2C+B+V">B. V. Kheswa</a>, <a href="/search/nucl-ex?searchtype=author&query=Khumalo%2C+N+A">N. A. Khumalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamula%2C+T">T. Lamula</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2204.11724v3-abstract-short" style="display: inline;"> We have measured the gamma-ray line production cross sections in proton-induced nuclear reactions on various target nuclei abundant in astrophysical sites over the incident energy range of Ep = 30 - 200 MeV. We carried out experimental campaigns in joint collaboration at the K = 200 cyclotron of iThemba LABS using a high-energy resolution, high-efficiency detection array composed of 8 Compton-supp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11724v3-abstract-full').style.display = 'inline'; document.getElementById('2204.11724v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.11724v3-abstract-full" style="display: none;"> We have measured the gamma-ray line production cross sections in proton-induced nuclear reactions on various target nuclei abundant in astrophysical sites over the incident energy range of Ep = 30 - 200 MeV. We carried out experimental campaigns in joint collaboration at the K = 200 cyclotron of iThemba LABS using a high-energy resolution, high-efficiency detection array composed of 8 Compton-suppressed clover detectors comprising 32 HP-Ge crystals for recording the gamma-ray spectra. In the current paper, we focus on de-excitation lines produced in proton irradiations of natC and Mylar targets. In particular, on the prominent 4.439 and 6.129 MeV lines of $^{12}$C and $^{16}$O which are among the strongest lines emitted in solar flares and in interactions of low-energy cosmic rays with the gas and dust of the inner galaxy. We report new gamma-ray production experimental cross section data for ten nuclear lines that we compare to previous low-energy data sets from the literature, to the predictions of the TALYS code of modern nuclear reactions and to a semi-empirical compilation. In first approach, performing calculations with default input parameters of TALYS we observed substantial deviations between the predicted cross sections and experimental data. Then, using modified optical model potential and nuclear level deformation parameters as input data we generated theoretical excitation functions for the above two main lines fully consistent with experimental data. In contrast, the experimental data sets for the other eight analyzed lines from the two proton-irradiated targets exhibit significant deviations with the predicted cross section values. We also report line-shape experimental data for the line complex observed at $E_g$ = 4.44 MeV in irradiations of the two targets. Finally, we emphasize the astrophysical implications of our results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.11724v3-abstract-full').style.display = 'none'; document.getElementById('2204.11724v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 7 tables, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Physics A Volume 1032, April 2023, 122622 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.03411">arXiv:2201.03411</a> <span> [<a href="https://arxiv.org/pdf/2201.03411">pdf</a>, <a href="https://arxiv.org/format/2201.03411">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.105.015805">10.1103/PhysRevC.105.015805 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental study of the $^{30}$Si($^{3}$He,$d$)$^{31}$P reaction and thermonuclear reaction rate of $^{30}$Si($p$,$纬$)$^{31}$P </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Harrouz%2C+D+S">D. S. Harrouz</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L. Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Palmerini%2C+S">S. Palmerini</a>, <a href="/search/nucl-ex?searchtype=author&query=Pizzone%2C+R+G">R. G. Pizzone</a>, <a href="/search/nucl-ex?searchtype=author&query=Romano%2C+S">S. Romano</a>, <a href="/search/nucl-ex?searchtype=author&query=Tumino%2C+A">A. Tumino</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.03411v1-abstract-short" style="display: inline;"> [Background] Abundance anomalies in some globular clusters, such as the enhancement of potassium and the depletion of magnesium, can be explained in terms of an earlier generation of stars polluting the presently observed ones. It was shown that the potential range of temperatures and densities of the polluting sites depends on the strength of a few number of critical reaction rates. The reaction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03411v1-abstract-full').style.display = 'inline'; document.getElementById('2201.03411v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.03411v1-abstract-full" style="display: none;"> [Background] Abundance anomalies in some globular clusters, such as the enhancement of potassium and the depletion of magnesium, can be explained in terms of an earlier generation of stars polluting the presently observed ones. It was shown that the potential range of temperatures and densities of the polluting sites depends on the strength of a few number of critical reaction rates. The reaction has been identified as one of these important reactions. [Purpose] The key ingredient for evaluating the thermonuclear reaction rate is the strength of the resonances which, at low energy, are proportional to their proton width. Therefore the goal of this work is to determine the proton widths of unbound 31P states. [Method] States in 31P were studied at the Maier-Leibnitz-Laboratorium using the one-proton transfer reaction. Deuterons were detected with the Q3D magnetic spectrometer. Angular distribution and spectroscopic factors were extracted for 27 states, and proton widths and resonance strengths were calculated for the unbound states. [Results] Several unbound states have been observed for the first time in a one-proton transfer reaction. Above 20 MK, the reaction rate is now entirely estimated from the observed properties of states. The reaction rate uncertainty from all resonances other than the resonance has been reduced down to less than a factor of two above that temperature. The unknown spin and parity of the resonance dominates the uncertainty in the rate in the relevant temperature range. [Conclusion] The remaining source of uncertainty on the reaction rate comes from the unknown spin and parity of the resonance which can change the reaction rate by a factor of ten in the temperature range of interest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.03411v1-abstract-full').style.display = 'none'; document.getElementById('2201.03411v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.01513">arXiv:2201.01513</a> <span> [<a href="https://arxiv.org/pdf/2201.01513">pdf</a>, <a href="https://arxiv.org/format/2201.01513">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.129.122501">10.1103/PhysRevLett.129.122501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The structure of $^{36}$Ca under the Coulomb magnifying glass </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Lalanne%2C+L">L. Lalanne</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Poves%2C+A">A. Poves</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Koyama%2C+S">S. Koyama</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Roger%2C+T">T. Roger</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+D+O">F. De Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Kamalou%2C+O">O. Kamalou</a>, <a href="/search/nucl-ex?searchtype=author&query=Kitamura%2C+N">N. Kitamura</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Mauss%2C+B">B. Mauss</a>, <a href="/search/nucl-ex?searchtype=author&query=Morfouace%2C+P">P. Morfouace</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.01513v2-abstract-short" style="display: inline;"> Detailed spectroscopy of the neutron-deficient nucleus $^{36}$Ca was obtained up to 9 MeV using the $^{37}$Ca($p$,$d$)$^{36}$Ca and the $^{38}$Ca($p$,$t$)$^{36}$Ca transfer reactions. The radioactive nuclei, produced by the LISE spectrometer at GANIL, interacted with the protons of the liquid Hydrogen target CRYPTA, to produce light ejectiles (the deuteron $d$ or triton $t$) that were detected in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01513v2-abstract-full').style.display = 'inline'; document.getElementById('2201.01513v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01513v2-abstract-full" style="display: none;"> Detailed spectroscopy of the neutron-deficient nucleus $^{36}$Ca was obtained up to 9 MeV using the $^{37}$Ca($p$,$d$)$^{36}$Ca and the $^{38}$Ca($p$,$t$)$^{36}$Ca transfer reactions. The radioactive nuclei, produced by the LISE spectrometer at GANIL, interacted with the protons of the liquid Hydrogen target CRYPTA, to produce light ejectiles (the deuteron $d$ or triton $t$) that were detected in the MUST2 detector array, in coincidence with the heavy residues %identified by a zero degree detection system. %States have been measured up to 9 MeV. Our main findings are: i) a similar shift in energy for the 1$^+_1$ and 2$^+_1$ states by about -250 keV, as compared to the mirror nucleus $^{36}$S, ii) the discovery of an intruder 0$^+_2$ state at 2.83(13) MeV, which appears below the first 2$^+$ state, in contradiction with the situation in $^{36}$S, and iii) a tentative 0$^+_3$ state at 4.83(17) MeV, proposed to exhibit a bubble structure with two neutron vacancies in the 2s$_{1/2}$ orbit. The inversion between the 0$^+_2$ and 2$^+_1$ states is due to the large mirror energy difference (MED) of -516(130) keV for the former. This feature is reproduced by Shell Model (SM) calculations, using the $sd$-$pf$ valence space, predicting an almost pure intruder nature for the 0$^+_2$ state, with two protons (neutrons) being excited across the $Z$=20 magic closure in $^{36}$Ca ($^{36}$S). This mirror system has the largest MEDs ever observed, if one excludes the few cases induced by the effect of the continuum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01513v2-abstract-full').style.display = 'none'; document.getElementById('2201.01513v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper of 5 pages, 3 figures. Contains also a supplementary material of 3 pages and 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.14412">arXiv:2111.14412</a> <span> [<a href="https://arxiv.org/pdf/2111.14412">pdf</a>, <a href="https://arxiv.org/format/2111.14412">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> Narrow resonances in the continuum of the unbound nucleus $^{15}$F </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Mercenne%2C+A">A. Mercenne</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Michel%2C+N">N. Michel</a>, <a href="/search/nucl-ex?searchtype=author&query=P%C5%82oszajczak%2C+M">M. P艂oszajczak</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Ramos%2C+D">D. Ramos</a>, <a href="/search/nucl-ex?searchtype=author&query=Rejmund%2C+M">M. Rejmund</a>, <a href="/search/nucl-ex?searchtype=author&query=Dudouet%2C+J">J. Dudouet</a>, <a href="/search/nucl-ex?searchtype=author&query=Ackermann%2C+D">D. Ackermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Assun%C3%A7%C3%A3o%2C+M">M. Assun莽茫o</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Benzoni%2C+G">G. Benzoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Boston%2C+A+J">A. J. Boston</a>, <a href="/search/nucl-ex?searchtype=author&query=C%C3%A1ceres%2C+L">L. C谩ceres</a>, <a href="/search/nucl-ex?searchtype=author&query=Cederwall%2C+B">B. Cederwall</a>, <a href="/search/nucl-ex?searchtype=author&query=Celikovic%2C+I">I. Celikovic</a> , et al. (78 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.14412v1-abstract-short" style="display: inline;"> The structure of the unbound $^{15}$F nucleus is investigated using the inverse kinematics resonant scattering of a radioactive $^{14}$O beam impinging on a CH$_2$ target. The analysis of $^{1}$H($^{14}$O,p)$^{14}$O and $^{1}$H($^{14}$O,2p)$^{13}$N reactions allowed the confirmation of the previously observed narrow $1/2^{-}$ resonance, near the two-proton decay threshold, and the identification o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14412v1-abstract-full').style.display = 'inline'; document.getElementById('2111.14412v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14412v1-abstract-full" style="display: none;"> The structure of the unbound $^{15}$F nucleus is investigated using the inverse kinematics resonant scattering of a radioactive $^{14}$O beam impinging on a CH$_2$ target. The analysis of $^{1}$H($^{14}$O,p)$^{14}$O and $^{1}$H($^{14}$O,2p)$^{13}$N reactions allowed the confirmation of the previously observed narrow $1/2^{-}$ resonance, near the two-proton decay threshold, and the identification of two new narrow 5/2$^{-}$ and 3/2$^{-}$ resonances. The newly observed levels decay by 1p emission to the ground of $^{14}$O, and by sequential 2p emission to the ground state (g.s.) of $^{13}$N via the $1^-$ resonance of $^{14}$O. Gamow shell model (GSM) analysis of the experimental data suggests that the wave functions of the 5/2$^{-}$ and 3/2$^{-}$ resonances may be collectivized by the continuum coupling to nearby 2p- and 1p- decay channels. The observed excitation function $^{1}$H($^{14}$O,p)$^{14}$O and resonance spectrum in $^{15}$F are well reproduced in the unified framework of the GSM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14412v1-abstract-full').style.display = 'none'; document.getElementById('2111.14412v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.02898">arXiv:2111.02898</a> <span> [<a href="https://arxiv.org/pdf/2111.02898">pdf</a>, <a href="https://arxiv.org/format/2111.02898">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Pulse shape discrimination for GRIT: beam test of a new integrated charge and current preamplifier coupled with high granularity Silicon detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Dormard%2C+J+-">J. -J. Dormard</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Grassi%2C+L">L. Grassi</a>, <a href="/search/nucl-ex?searchtype=author&query=Rauly%2C+E">E. Rauly</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Brulin%2C+G">G. Brulin</a>, <a href="/search/nucl-ex?searchtype=author&query=Chabot%2C+M">M. Chabot</a>, <a href="/search/nucl-ex?searchtype=author&query=Coacolo%2C+J+-">J. -L. Coacolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Genolini%2C+B">B. Genolini</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Barkach%2C+T+I">T. Id Barkach</a>, <a href="/search/nucl-ex?searchtype=author&query=Rindel%2C+E">E. Rindel</a>, <a href="/search/nucl-ex?searchtype=author&query=Rosier%2C+P">Ph. Rosier</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Wanlin%2C+E">E. Wanlin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2111.02898v1-abstract-short" style="display: inline;"> The GRIT (Granularity, Resolution, Identification, Transparency) Silicon array is intended to measure direct reactions. Its design is based on several layers (three layers in the forward direction, two backward) of custom-made trapezoidal and square detectors. The first stage is 500 渭m thick and features 128x128 orthogonal strips. Pulse shape analysis for particle identification is implemented for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02898v1-abstract-full').style.display = 'inline'; document.getElementById('2111.02898v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.02898v1-abstract-full" style="display: none;"> The GRIT (Granularity, Resolution, Identification, Transparency) Silicon array is intended to measure direct reactions. Its design is based on several layers (three layers in the forward direction, two backward) of custom-made trapezoidal and square detectors. The first stage is 500 渭m thick and features 128x128 orthogonal strips. Pulse shape analysis for particle identification is implemented for this first layer. Given the compacity of this array and the large number of channels involved (>7,500), an integrated preamplifier, iPACI, that gives charge and current information has been developed in the AMS 0.35 渭m BiCMOS technology. The design specifications and results of the test bench are presented. Considering an energy range of 50 MeV and an energy resolution (FWHM) of 12 keV (FWHM) for the preamplifier, the energy resolution for one strip obtained from alpha source measurement in real conditions is 35 keV. The current output bandwidth is measured at 130 MHz for small signals and the power consumption reaches 40 mW per detector channel. A first beam test was performed coupling a nTD trapezoidal double-sided stripped Silicon detector of GRIT with the iPACI preamplifier and a 64-channel digitizer. Z=1 particles are discriminated with pulse shape analysis technique down to 2 MeV for protons, 2.5 MeV for deuterons and 3 MeV for tritons. The effect of the strip length due to the trapezoidal shape of the detector is investigated on both the N- and the P-side, showing no significant impact. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02898v1-abstract-full').style.display = 'none'; document.getElementById('2111.02898v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.06145">arXiv:2108.06145</a> <span> [<a href="https://arxiv.org/pdf/2108.06145">pdf</a>, <a href="https://arxiv.org/format/2108.06145">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The 27Al(p,a)24Mg reaction at astrophysical energies studied by means of the Trojan Horse Method applied to the 2H(27Al,a24Mg)n reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Palmerini%2C+S">Sara Palmerini</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">Marco La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">Fairouz Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Acosta%2C+L">Luis Acosta</a>, <a href="/search/nucl-ex?searchtype=author&query=Alba%2C+R">Rosa Alba</a>, <a href="/search/nucl-ex?searchtype=author&query=Burjan%2C+V">Vaclav Burjan</a>, <a href="/search/nucl-ex?searchtype=author&query=Chavez%2C+E">Efrain Chavez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">Silvio Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Cvetinovic%2C+A">Alexandra Cvetinovic</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Agata%2C+G">Giuseppe D'Agata</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Sereville%2C+N">Nicolas De Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Pietro%2C+A">Alessia Di Pietro</a>, <a href="/search/nucl-ex?searchtype=author&query=Figuera%2C+P">Pierpaolo Figuera</a>, <a href="/search/nucl-ex?searchtype=author&query=Fullop%2C+Z">Zsolt Fullop</a>, <a href="/search/nucl-ex?searchtype=author&query=Rios%2C+K+D+L">Karen De Los Rios</a>, <a href="/search/nucl-ex?searchtype=author&query=Guardo%2C+G+L">Giovanni Luca Guardo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gulino%2C+M">Marisa Gulino</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">Seiya Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiss%2C+G">Gabor Kiss</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Commara%2C+M">Marco La Commara</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">Livio Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Manic%C3%B2%2C+C+M+G">Concetta Maiolino Giulio Manic貌</a>, <a href="/search/nucl-ex?searchtype=author&query=Matei%2C+C">Catalin Matei</a>, <a href="/search/nucl-ex?searchtype=author&query=Mazzocco%2C+M">Marco Mazzocco</a>, <a href="/search/nucl-ex?searchtype=author&query=Mrazek%2C+J">Jaromir Mrazek</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2108.06145v1-abstract-short" style="display: inline;"> The 27Al(p,a)24Mg reaction, which drives the destruction of 27Al and the production of 24Mg in stellar hydrogen burning, has been investigated via the Trojan Horse Method (THM) by measuring the 2H(27Al,a24Mg)n three-body reaction. The experiment covered a broad energy range (-0.5 MeV < E_cm < 1.5 MeV), aiming to investigate those of interest for astrophysics.The results confirm the THM as a valuab… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06145v1-abstract-full').style.display = 'inline'; document.getElementById('2108.06145v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.06145v1-abstract-full" style="display: none;"> The 27Al(p,a)24Mg reaction, which drives the destruction of 27Al and the production of 24Mg in stellar hydrogen burning, has been investigated via the Trojan Horse Method (THM) by measuring the 2H(27Al,a24Mg)n three-body reaction. The experiment covered a broad energy range (-0.5 MeV < E_cm < 1.5 MeV), aiming to investigate those of interest for astrophysics.The results confirm the THM as a valuable technique for the experimental study of fusion reactions at very low energies and suggest the presence of a rich pattern of resonances in the energy region close to the Gamow window of stellar hydrogen burning (70-120 keV), with potential impact on astrophysics. To estimate such an impact a second run of the experiment is needed, since the background due the three-body reaction hampered to collect enough data to resolve the resonant structures and extract the reaction rate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.06145v1-abstract-full').style.display = 'none'; document.getElementById('2108.06145v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, accepted for publication by EPJ Plus</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.13228">arXiv:2107.13228</a> <span> [<a href="https://arxiv.org/pdf/2107.13228">pdf</a>, <a href="https://arxiv.org/format/2107.13228">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3389/fphy.2020.602920">10.3389/fphy.2020.602920 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Transfer reactions as a Tool in Nuclear Astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">Fa茂rouz Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">Nicolas de S茅r茅ville</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.13228v1-abstract-short" style="display: inline;"> Nuclear reaction rates are one of the most important ingredients in describing how stars evolve. The study of the nuclear reactions involved in different astrophysical sites is thus mandatory to address most questions in nuclear astrophysics. Direct measurements of the cross-sections at stellar energies are very challenging - if at all possible. This is essentially due to the very low cross-sectio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13228v1-abstract-full').style.display = 'inline'; document.getElementById('2107.13228v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.13228v1-abstract-full" style="display: none;"> Nuclear reaction rates are one of the most important ingredients in describing how stars evolve. The study of the nuclear reactions involved in different astrophysical sites is thus mandatory to address most questions in nuclear astrophysics. Direct measurements of the cross-sections at stellar energies are very challenging - if at all possible. This is essentially due to the very low cross-sections of the reactions of interest (especially when it involves charged particles), and/or to the radioactive nature of many key nuclei. In order to overcome these difficulties, various indirect methods such as the transfer reaction method at energies above or near the Coulomb barrier are used to measure the spectroscopic properties of the involved compound nucleus that are needed to calculate cross-sections or reaction rates of astrophysical interest. In this review, the basic features of the transfer reaction method and the theoretical concept behind are first discussed, then the method is illustrated with recent performed experimental studies of key reactions in nuclear astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.13228v1-abstract-full').style.display = 'none'; document.getElementById('2107.13228v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> https://www.frontiersin.org/articles/10.3389/fphy.2020.602920/full </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.04317">arXiv:2107.04317</a> <span> [<a href="https://arxiv.org/pdf/2107.04317">pdf</a>, <a href="https://arxiv.org/format/2107.04317">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.103.055809">10.1103/PhysRevC.103.055809 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evaluation of the $^{35}$K($p$,$纬$)$^{36}$Ca reaction rate using the $^{37}$Ca($p$,$d$)$^{36}$Ca transfer reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Lalanne%2C+L">L. Lalanne</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Koyama%2C+S">S. Koyama</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+D+O">F. De Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Kamalou%2C+O">O. Kamalou</a>, <a href="/search/nucl-ex?searchtype=author&query=Kitamura%2C+N">N. Kitamura</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Mauss%2C+B">B. Mauss</a>, <a href="/search/nucl-ex?searchtype=author&query=Morfouace%2C+P">P. Morfouace</a>, <a href="/search/nucl-ex?searchtype=author&query=Niikura%2C+M">M. Niikura</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2107.04317v1-abstract-short" style="display: inline;"> A recent sensitivity study has shown that the $^{35}$K$(p,纬)^{36}$Ca reaction is one of the ten $(p,纬)$ reaction rates that could significantly impact the shape of the calculated X-ray burst light curve. In this work, we propose to reinvestigate the $^{35}$K$(p,纬)^{36}$Ca reaction rate, as well as related uncertainties, by determining the energies and decay branching ratios of $^{36}$Ca levels, wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04317v1-abstract-full').style.display = 'inline'; document.getElementById('2107.04317v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.04317v1-abstract-full" style="display: none;"> A recent sensitivity study has shown that the $^{35}$K$(p,纬)^{36}$Ca reaction is one of the ten $(p,纬)$ reaction rates that could significantly impact the shape of the calculated X-ray burst light curve. In this work, we propose to reinvestigate the $^{35}$K$(p,纬)^{36}$Ca reaction rate, as well as related uncertainties, by determining the energies and decay branching ratios of $^{36}$Ca levels, within the Gamow window, in the 0.5 to 2 GK X-ray burst temperature range. These properties were studied using the one neutron pick-up transfer reaction $^{37}$Ca$(p,d)^{36}$Ca in inverse kinematics using a radioactive beam of $^{37}$Ca at 48 MeV nucleon$^{-1}$. The experiment performed at GANIL, used the liquid Hydrogen target CRYPTA, the MUST2 detector array for the detection of the light charged particles and a zero degree detection system for the outgoing heavy ions. The atomic mass of $^{36}$Ca is confirmed and new resonances have been proposed together with their proton decay branching ratios. This spectroscopic information, used in combination with recent theoretical predictions for the $纬$-width, were used to calculate the $^{35}$K$(p,纬)^{36}$Ca reaction rate. The recommended rate of the present work was obtain within a uncertainty factor of 2 at 1 sigma. This is consistent, with the previous estimate in the X-ray burst temperature range. A large increase of the reaction rate was found at higher temperatures due to two newly discovered resonances. The $^{35}$K$(p,纬)^{36}$Ca thermonuclear reaction rate is now well constrained by the present work in a broad range of temperatures. Our results show that the $^{35}$K$(p,纬)^{36}$Ca reaction does not affect the shape of the X-ray burst light curve, and that it can be removed from the list of the few influential proton radiative captures reactions having a strong impact on the light curve. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04317v1-abstract-full').style.display = 'none'; document.getElementById('2107.04317v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published 13 May 2021 in PRC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 103, 055809 , 2021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.01848">arXiv:2106.01848</a> <span> [<a href="https://arxiv.org/pdf/2106.01848">pdf</a>, <a href="https://arxiv.org/format/2106.01848">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.104.054308">10.1103/PhysRevC.104.054308 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron occupancies and single-particle energies across the stable tin isotopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Szwec%2C+S+V">S. V. Szwec</a>, <a href="/search/nucl-ex?searchtype=author&query=Sharp%2C+D+K">D. K. Sharp</a>, <a href="/search/nucl-ex?searchtype=author&query=Kay%2C+B+P">B. P. Kay</a>, <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+S+J">S. J. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiffer%2C+J+P">J. P. Schiffer</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Binnersley%2C+C">C. Binnersley</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Ruiz%2C+R+F+G">R. F. Garcia Ruiz</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Vernon%2C+A">A. Vernon</a>, <a href="/search/nucl-ex?searchtype=author&query=Wilkins%2C+S">S. Wilkins</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2106.01848v1-abstract-short" style="display: inline;"> The occupancies and vacancies of the valence neutron orbitals across the stable tin isotopic chain from $112\leq A\leq 124$ have been determined. These were inferred from the cross sections of neutron-adding and -removing reactions. In each case, the reactions were chosen to have good angular-momentum matching for transfer to the low- and high-$\ell$ orbitals present in this valence space. These n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01848v1-abstract-full').style.display = 'inline'; document.getElementById('2106.01848v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.01848v1-abstract-full" style="display: none;"> The occupancies and vacancies of the valence neutron orbitals across the stable tin isotopic chain from $112\leq A\leq 124$ have been determined. These were inferred from the cross sections of neutron-adding and -removing reactions. In each case, the reactions were chosen to have good angular-momentum matching for transfer to the low- and high-$\ell$ orbitals present in this valence space. These new data are compared to older systematic studies. The effective single-neutron energies are determined by combining information from energy centroids determined from the adding and removing reactions. Two of the five orbitals are nearly degenerate, below $N=64$, and approximately two MeV more bound than the other three, which are also degenerate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.01848v1-abstract-full').style.display = 'none'; document.getElementById('2106.01848v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.10708">arXiv:2104.10708</a> <span> [<a href="https://arxiv.org/pdf/2104.10708">pdf</a>, <a href="https://arxiv.org/format/2104.10708">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2022.137057">10.1016/j.physletb.2022.137057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron-proton pairing in the N=Z radioactive fp-shell nuclei 56Ni and 52Fe probed by pair transfer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Crom%2C+B+L">B. Le Crom</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y. Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Sagawa%2C+H">H. Sagawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+T">T. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Honma%2C+M">M. Honma</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+N+L">N. L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W+N">W. N. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Clement%2C+E">E. Clement</a>, <a href="/search/nucl-ex?searchtype=author&query=Caceres%2C+L">L. Caceres</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/nucl-ex?searchtype=author&query=De+France%2C+G">G. De France</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=De+S%C3%A9r%C3%A9ville%2C+N">N. De S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Fisichella%2C+M">M. Fisichella</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Georgiadou%2C+A">A. Georgiadou</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillibert%2C+A">A. Gillibert</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.10708v1-abstract-short" style="display: inline;"> The isovector and isoscalar components of neutron-proton pairing are investigated in the N=Z unstable nuclei of the \textit{fp}-shell through the two-nucleon transfer reaction (p,$^3$He) in inverse kinematics. The combination of particle and gamma-ray detection with radioactive beams of $^{56}$Ni and $^{52}$Fe, produced by fragmentation at the GANIL/LISE facility, made it possible to carry out thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10708v1-abstract-full').style.display = 'inline'; document.getElementById('2104.10708v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.10708v1-abstract-full" style="display: none;"> The isovector and isoscalar components of neutron-proton pairing are investigated in the N=Z unstable nuclei of the \textit{fp}-shell through the two-nucleon transfer reaction (p,$^3$He) in inverse kinematics. The combination of particle and gamma-ray detection with radioactive beams of $^{56}$Ni and $^{52}$Fe, produced by fragmentation at the GANIL/LISE facility, made it possible to carry out this study for the first time in a closed and an open-shell nucleus in the \textit{fp}-shell. The transfer cross-sections for ground-state to ground-state (J=0$^+$,T=1) and to the first (J=1$^+$,T=0) state were extracted for both cases together with the transfer cross-section ratios $蟽$(0$^+$,T=1) /$蟽$(1$^+$,T=0). They are compared with second-order distorted-wave born approximation (DWBA) calculations. The enhancement of the ground-state to ground-state pair transfer cross-section close to mid-shell, in $^{52}$Fe, points towards a superfluid phase in the isovector channel. For the "deuteron-like" transfer, very low cross-sections to the first (J=1$^+$,T=0) state were observed both for \Ni\phe\, and \Fe\phe\, and are related to a strong hindrance of this channel due to spin-orbit effect. No evidence for an isoscalar deuteron-like condensate is observed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10708v1-abstract-full').style.display = 'none'; document.getElementById('2104.10708v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.10707">arXiv:2104.10707</a> <span> [<a href="https://arxiv.org/pdf/2104.10707">pdf</a>, <a href="https://arxiv.org/format/2104.10707">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2021.165743">10.1016/j.nima.2021.165743 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MUGAST-AGATA-VAMOS campaign : set-up and performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Ramos%2C+D">D. Ramos</a>, <a href="/search/nucl-ex?searchtype=author&query=Raggio%2C+A">A. Raggio</a>, <a href="/search/nucl-ex?searchtype=author&query=Zanon%2C+I">I. Zanon</a>, <a href="/search/nucl-ex?searchtype=author&query=Galtarossa%2C+F">F. Galtarossa</a>, <a href="/search/nucl-ex?searchtype=author&query=Lenain%2C+C">C. Lenain</a>, <a href="/search/nucl-ex?searchtype=author&query=Casal%2C+J">J. Casal</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Mengoni%2C+D">D. Mengoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y. Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Brugnara%2C+D">D. Brugnara</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W">W. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Oliveira%2C+F">F. de Oliveira</a>, <a href="/search/nucl-ex?searchtype=author&query=De+S%C3%A9r%C3%A9ville%2C+N">N. De S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Didierjean%2C+F">F. Didierjean</a>, <a href="/search/nucl-ex?searchtype=author&query=Diget%2C+C+A">C. Aa. Diget</a>, <a href="/search/nucl-ex?searchtype=author&query=Dudouet%2C+J">J. Dudouet</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Foug%C3%A8res%2C+C">C. Foug猫res</a>, <a href="/search/nucl-ex?searchtype=author&query=Fr%C3%A9mont%2C+G">G. Fr茅mont</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.10707v1-abstract-short" style="display: inline;"> The MUGAST-AGATA-VAMOS set-up at GANIL combines the MUGAST highly-segmented silicon array with the state-of-the-art AGATA array and the large acceptance VAMOS spectrometer. The mechanical and electronics integration copes with the constraints of maximum efficiency for each device, in particular 纬-ray transparency for the silicon array. This complete set-up offers a unique opportunity to perform ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10707v1-abstract-full').style.display = 'inline'; document.getElementById('2104.10707v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.10707v1-abstract-full" style="display: none;"> The MUGAST-AGATA-VAMOS set-up at GANIL combines the MUGAST highly-segmented silicon array with the state-of-the-art AGATA array and the large acceptance VAMOS spectrometer. The mechanical and electronics integration copes with the constraints of maximum efficiency for each device, in particular 纬-ray transparency for the silicon array. This complete set-up offers a unique opportunity to perform exclusive measurements of direct reactions with the radioactive beams from the SPIRAL1 facility. The performance of the set-up is described through its commissioning and two examples of transfer reactions measured during the campaign. High accuracy spectroscopy of the nuclei of interest, including cross-sections and angular distributions, is achieved through the triple-coincidence measurement. In addition, the correction from Doppler effect of the 纬-ray energies is improved by the detection of the light particles and the use of two-body kinematics and a full rejection of the background contributions is obtained through the identification of heavy residues. Moreover, the system can handle high intensity beams (up to 108 pps). The particle identification based on the measurement of the time-of-flight between MUGAST and VAMOS and the reconstruction of the trajectories is investigated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10707v1-abstract-full').style.display = 'none'; document.getElementById('2104.10707v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 18 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nuclear Inst. and Methods in Physics Research, A 1014 (2021) 165743 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02132">arXiv:2101.02132</a> <span> [<a href="https://arxiv.org/pdf/2101.02132">pdf</a>, <a href="https://arxiv.org/format/2101.02132">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-021-00410-1">10.1140/epja/s10050-021-00410-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing nuclear forces beyond the nuclear drip line: The cases of $^{16}$F and $^{15}$F </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Girard-Alcindor%2C+V">V. Girard-Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Ackermann%2C+D">D. Ackermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Angelique%2C+J+C">J. C. Angelique</a>, <a href="/search/nucl-ex?searchtype=author&query=Assie%2C+M">M. Assie</a>, <a href="/search/nucl-ex?searchtype=author&query=Assuncao%2C+M">M. Assuncao</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Berthoumieux%2C+E">E. Berthoumieux</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Caceres%2C+L">L. Caceres</a>, <a href="/search/nucl-ex?searchtype=author&query=Celikovic%2C+I">I. Celikovic</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciemala%2C+M">M. Ciemala</a>, <a href="/search/nucl-ex?searchtype=author&query=Chudoba%2C+V">V. Chudoba</a>, <a href="/search/nucl-ex?searchtype=author&query=Agata%2C+G+D">G. D Agata</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Grancey%2C+F">F. de Grancey</a>, <a href="/search/nucl-ex?searchtype=author&query=Dumitru%2C+G">G. Dumitru</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Fougeres%2C+C">C. Fougeres</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Georgiadou%2C+A">A. Georgiadou</a>, <a href="/search/nucl-ex?searchtype=author&query=Grevy%2C+S">S. Grevy</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a> , et al. (31 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.02132v1-abstract-short" style="display: inline;"> The unbound proton-rich nuclei $^{16}$F and $^{15}$F are investigated experimentally and theoretically. Several experiments using the resonant elastic scattering method were performed at GANIL with radioactive beams to determine the properties of the low lying states of these nuclei. Strong asymmetry between $^{16}$F-$^{16}$N and $^{15}$F-$^{15}$C mirror nuclei is observed. The strength of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02132v1-abstract-full').style.display = 'inline'; document.getElementById('2101.02132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02132v1-abstract-full" style="display: none;"> The unbound proton-rich nuclei $^{16}$F and $^{15}$F are investigated experimentally and theoretically. Several experiments using the resonant elastic scattering method were performed at GANIL with radioactive beams to determine the properties of the low lying states of these nuclei. Strong asymmetry between $^{16}$F-$^{16}$N and $^{15}$F-$^{15}$C mirror nuclei is observed. The strength of the $nucleon-nucleon$ effective interaction involving the loosely bound proton in the $s_{1/2}$ orbit is significantly modified with respect to their mirror nuclei $^{16}$N and $^{15}$C. The reduction of the effective interaction is estimated by calculating the interaction energies with a schematic zero-range force. It is found that, after correcting for the effects due to changes in the radial distribution of the single-particle wave functions, the mirror symmetry of the $n-p$ interaction is preserved between $^{16}$F and $^{16}$N, while a difference of 63\% is measured between the $p-p$ versus $n-n$ interactions in the second excited state of $^{15}$F and $^{15}$C nuclei. Several explanations are proposed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02132v1-abstract-full').style.display = 'none'; document.getElementById('2101.02132v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. A 57, 93 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13222">arXiv:2011.13222</a> <span> [<a href="https://arxiv.org/pdf/2011.13222">pdf</a>, <a href="https://arxiv.org/format/2011.13222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.103.015807">10.1103/PhysRevC.103.015807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-threshold states in $^{19}$Ne relevant to $^{18}$F(p,$伪$)$^{15}$O </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Riley%2C+J+E">J. E. Riley</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Boulay%2C+F">F. Boulay</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Garg%2C+R">R. Garg</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillespie%2C+S+A">S. A. Gillespie</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimaraes%2C+V">V. Guimaraes</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hubbard%2C+N">N. Hubbard</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Remadi%2C+A">A. Remadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Perrot%2C+L">L. Perrot</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Verde%2C+G">G. Verde</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.13222v1-abstract-short" style="display: inline;"> Classical novae result from thermonuclear explosions producing several $纬$-ray emitters which are prime targets for satellites observing in the MeV range. The early 511 keV gamma-ray emission depends critically on the $^{18}$F(p,$伪$)$^{15}$O reaction rate which, despite many experimental and theoretical efforts, still remains uncertain. One of the main uncertainties in the $^{18}$F(p,$伪$)$^{15}$O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13222v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13222v1-abstract-full" style="display: none;"> Classical novae result from thermonuclear explosions producing several $纬$-ray emitters which are prime targets for satellites observing in the MeV range. The early 511 keV gamma-ray emission depends critically on the $^{18}$F(p,$伪$)$^{15}$O reaction rate which, despite many experimental and theoretical efforts, still remains uncertain. One of the main uncertainties in the $^{18}$F(p,$伪$)$^{15}$O reaction rate is the contribution in the Gamow window of interference between sub-threshold $^{19}$Ne states and known broad states at higher energies. Therefore the goal of this work is to clarify the existence and the nature of these sub-threshold states. States in the $^{19}$Ne compound nucleus were studied at the Tandem-ALTO facility using the $^{19}$F($^3$He,t)$^{19}$Ne charge exchange reaction. Tritons were detected with an Enge Split-pole spectrometer while decaying protons or $伪$-particles from unbound $^{19}$Ne states were collected, in coincidence, with a double-sided silicon strip detector array. Angular correlations were extracted and constraints on the spin and parity of decaying states established. The coincidence yield at $E_x$ = 6.29 MeV was observed to be high spin, supporting the conclusion that it is indeed a doublet consisting of high spin and low spin components. Evidence for a broad, low spin state was observed around 6 MeV. Branching ratios were extracted for several states above the proton threshold and were found to be consistent with the literature. R-matrix calculations show the relative contribution of sub-threshold states to the astrophysically important energy region above the proton threshold. The levels schemes of $^{19}$Ne and $^{19}$F are still not sufficiently well known and further studies of the analogue assignments are needed. The tentative broad state at 6 MeV may only play a role if the reduced proton width is large. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13222v1-abstract-full').style.display = 'none'; document.getElementById('2011.13222v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.06101">arXiv:2011.06101</a> <span> [<a href="https://arxiv.org/pdf/2011.06101">pdf</a>, <a href="https://arxiv.org/ps/2011.06101">ps</a>, <a href="https://arxiv.org/format/2011.06101">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2020.135939">10.1016/j.physletb.2020.135939 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-lying single-particle structure of 17C and the N = 14 sub-shell closure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Pereira-L%C3%B3pez%2C+X">X. Pereira-L贸pez</a>, <a href="/search/nucl-ex?searchtype=author&query=Fern%C3%A1ndez-Dom%C3%ADnguez%2C+B">B. Fern谩ndez-Dom铆nguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+N+L">N. L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Orr%2C+N+A">N. A. Orr</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W+N">W. N. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Bailey%2C+S">S. Bailey</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y. Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Borcea%2C+R">R. Borcea</a>, <a href="/search/nucl-ex?searchtype=author&query=Caama%C3%B1o%2C+M">M. Caama帽o</a>, <a href="/search/nucl-ex?searchtype=author&query=Caceres%2C+L">L. Caceres</a>, <a href="/search/nucl-ex?searchtype=author&query=Cl%C3%A9ment%2C+E">E. Cl茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Corsi%2C+A">A. Corsi</a>, <a href="/search/nucl-ex?searchtype=author&query=Curtis%2C+N">N. Curtis</a>, <a href="/search/nucl-ex?searchtype=author&query=Deshayes%2C+Q">Q. Deshayes</a>, <a href="/search/nucl-ex?searchtype=author&query=Farget%2C+F">F. Farget</a>, <a href="/search/nucl-ex?searchtype=author&query=Fisichella%2C+M">M. Fisichella</a>, <a href="/search/nucl-ex?searchtype=author&query=de+France%2C+G">G. de France</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Freer%2C+M">M. Freer</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillibert%2C+A">A. Gillibert</a>, <a href="/search/nucl-ex?searchtype=author&query=Grinyer%2C+G+F">G. F. Grinyer</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.06101v1-abstract-short" style="display: inline;"> The first investigation of the single-particle structure of the bound states of 17C, via the d(16C, p) transfer reaction, has been undertaken. The measured angular distributions confirm the spin-parity assignments of 1/2+ and 5/2+ for the excited states located at 217 and 335 keV, respectively. The spectroscopic factors deduced for these states exhibit a marked single-particle character, in agreem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06101v1-abstract-full').style.display = 'inline'; document.getElementById('2011.06101v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06101v1-abstract-full" style="display: none;"> The first investigation of the single-particle structure of the bound states of 17C, via the d(16C, p) transfer reaction, has been undertaken. The measured angular distributions confirm the spin-parity assignments of 1/2+ and 5/2+ for the excited states located at 217 and 335 keV, respectively. The spectroscopic factors deduced for these states exhibit a marked single-particle character, in agreement with shell model and particle-core model calculations, and combined with their near degeneracy in energy provide clear evidence for the absence of the N = 14 sub-shell closure. The very small spectroscopic factor found for the 3/2+ ground state is consistent with theoretical predictions and indicates that the 谓1d3/2 strength is carried by unbound states. With a dominant l = 0 valence neutron configuration and a very low separation energy, the 1/2+ excited state is a one-neutron halo candidate. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06101v1-abstract-full').style.display = 'none'; document.getElementById('2011.06101v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 5 figures, Accepted for publication in Physics Letters B</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.03965">arXiv:2007.03965</a> <span> [<a href="https://arxiv.org/pdf/2007.03965">pdf</a>, <a href="https://arxiv.org/ps/2007.03965">ps</a>, <a href="https://arxiv.org/format/2007.03965">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.103.035804">10.1103/PhysRevC.103.035804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Charged-particle branching ratios above the neutron threshold in $^{19}$F: constraining $^{15}$N production in core-collapse supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Alcindor%2C+V">V. Alcindor</a>, <a href="/search/nucl-ex?searchtype=author&query=%C3%A9%2C+M+A">M. Assi 茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Chabot%2C+D+B+M">D. Beaumel M. Chabot</a>, <a href="/search/nucl-ex?searchtype=author&query=Degerlier%2C+M">M. Degerlier</a>, <a href="/search/nucl-ex?searchtype=author&query=Delafosse%2C+C">C. Delafosse</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Garg%2C+R">R. Garg</a>, <a href="/search/nucl-ex?searchtype=author&query=Georgiadou%2C+A">A. Georgiadou</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillespie%2C+S+A">S. A. Gillespie</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimar%C3%A3es%2C+V">V. Guimar茫es</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Gottardo%2C+A">A. Gottardo</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Matea%2C+I">I. Matea</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.03965v4-abstract-short" style="display: inline;"> Spatially-correlated overabundances of $^{15}$N and $^{18}$O observed in some low-density graphite meteoritic grains have been connected to nucleosynthesis taking place in the helium-burning shell during core-collapse supernovae. Two of the reactions which have been identified as important to the final abundances of $^{15}$N and $^{18}$O are $^{18}$F($n,伪$)$^{15}$N and $^{18}$F($n,p$)$^{18}$O. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03965v4-abstract-full').style.display = 'inline'; document.getElementById('2007.03965v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.03965v4-abstract-full" style="display: none;"> Spatially-correlated overabundances of $^{15}$N and $^{18}$O observed in some low-density graphite meteoritic grains have been connected to nucleosynthesis taking place in the helium-burning shell during core-collapse supernovae. Two of the reactions which have been identified as important to the final abundances of $^{15}$N and $^{18}$O are $^{18}$F($n,伪$)$^{15}$N and $^{18}$F($n,p$)$^{18}$O. The relative strengths of the $^{18}$F($n,伪$)$^{15}$N and $^{18}$F($n,p$)$^{18}$O reactions depend on the relative $伪_0$ and $p_0$ decays from states above the neutron threshold in $^{19}$F in addition to other properties. Experimental data on the charged-particle decays from these highly excited states are lacking or inconsistent. Two experiments were performed using proton inelastic scattering from LiF targets and magnetic spectrographs. The first experiment used the high-resolution Q3D spectrograph at Munich to constrain properties of levels in $^{19}$F. A second experiment using the Orsay Split-Pole spectrograph and an array of silicon detectors was performed in order to measure the charged-particle decays of neutron-unbound levels in $^{19}$F. A number of levels in $^{19}$F have been identified along with their corresponding charged-particle decays. The first state above the neutron threshold which has an observed proton-decay branch to the ground state of $^{18}$O lies 68 keV above the neutron threshold while the $伪$-particle decays from the neutron-unbound levels are generally observed to be much stronger than the proton decays. Neutron-unbound levels in $^{19}$F are observed to decay predominantly by $伪$-particle emission, supporting the role of $^{18}$F($n,伪$)$^{15}$N in the production of $^{15}$N in the helium-burning shell of supernovae. Improved resonant-scattering reaction data are required in order to be able to determine the reaction rates accurately. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.03965v4-abstract-full').style.display = 'none'; document.getElementById('2007.03965v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, v3 more wrong affiliations</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 103, 035804 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.13589">arXiv:2006.13589</a> <span> [<a href="https://arxiv.org/pdf/2006.13589">pdf</a>, <a href="https://arxiv.org/format/2006.13589">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.102.035803">10.1103/PhysRevC.102.035803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evaluation of the $^{13}$N($伪$,p)$^{16}$O thermonuclear reaction rate and its impact on the isotopic composition of supernova grains </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawson%2C+T">T. Lawson</a>, <a href="/search/nucl-ex?searchtype=author&query=Pignatari%2C+M">M. Pignatari</a>, <a href="/search/nucl-ex?searchtype=author&query=Audouin%2C+L">L. Audouin</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Fortier%2C+S">S. Fortier</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Pellegriti%2C+M+G">M. G. Pellegriti</a>, <a href="/search/nucl-ex?searchtype=author&query=Stanoiu%2C+M">M. Stanoiu</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2006.13589v1-abstract-short" style="display: inline;"> It has been suggested that hydrogen ingestion into the helium shell of massive stars could lead to high $^{13}$C and $^{15}$N excesses when the shock of a core-collapse supernova passes through its helium shell. This prediction questions the origin of extremely high $^{13}$C and $^{15}$N abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13589v1-abstract-full').style.display = 'inline'; document.getElementById('2006.13589v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.13589v1-abstract-full" style="display: none;"> It has been suggested that hydrogen ingestion into the helium shell of massive stars could lead to high $^{13}$C and $^{15}$N excesses when the shock of a core-collapse supernova passes through its helium shell. This prediction questions the origin of extremely high $^{13}$C and $^{15}$N abundances observed in rare presolar SiC grains which is usually attributed to classical novae. In this context $^{13}$N($伪$,p)$^{16}$O the reaction plays an important role since it is in competition with $^{13}$N $尾^+$-decay to $^{13}$C. The $^{13}$N($伪$,p)$^{16}$O reaction rate used in stellar evolution calculations comes from the CF88 compilation with very scarce information on the origin of this rate. The goal of this work is to provide a recommended $^{13}$N($伪$,p)$^{16}$O reaction rate, based on available experimental data. Unbound nuclear states in the $^{17}$F compound nucleus were studied using the spectroscopic information of the analog states in $^{17}$O nucleus that were measured at the Alto facility using the $^{13}$C($^7$Li,t)$^{17}$O alpha-transfer reaction, and spectroscopic factors were derived using a DWBA analysis. This spectroscopic information was used to calculate a recommended $^{13}$N($伪$,p)$^{16}$O reaction rate with meaningful uncertainty using a Monte Carlo approach. The present $^{13}$N($伪$,p)$^{16}$O reaction rate is found to be within a factor of two of the previous evaluation, with a typical uncertainty of a factor 2-3. The source of this uncertainty comes from the three resonances at $E_r^{c.m.} = 221$, 741 and 959 keV. This new error estimation translates to an overall uncertainty in the $^{13}$C production of a factor of 50. The main source of uncertainty on the re-evaluated $^{13}$N($伪$,p)$^{16}$O reaction rate currently comes from the uncertain alpha-width of relevant $^{17}$F states. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.13589v1-abstract-full').style.display = 'none'; document.getElementById('2006.13589v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 102, 035803 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.07087">arXiv:2001.07087</a> <span> [<a href="https://arxiv.org/pdf/2001.07087">pdf</a>, <a href="https://arxiv.org/ps/2001.07087">ps</a>, <a href="https://arxiv.org/format/2001.07087">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.102.025802">10.1103/PhysRevC.102.025802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement and analysis of nuclear $纬$-ray production cross sections in proton interactions with Mg, Si and Fe nuclei abundant in astrophysical sites over the incident energy range $E=30-66$ MeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Yahia-Cherif%2C+W">W. Yahia-Cherif</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+E+A">E. A. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+J+J">J. J. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Belhout%2C+A">A. Belhout</a>, <a href="/search/nucl-ex?searchtype=author&query=Moussa%2C+D">D. Moussa</a>, <a href="/search/nucl-ex?searchtype=author&query=Papka%2C+P">P. Papka</a>, <a href="/search/nucl-ex?searchtype=author&query=Benhabiles%2C+H">H. Benhabiles</a>, <a href="/search/nucl-ex?searchtype=author&query=Bucher%2C+T+D">T. D. Bucher</a>, <a href="/search/nucl-ex?searchtype=author&query=Chafa%2C+A">A. Chafa</a>, <a href="/search/nucl-ex?searchtype=author&query=Conradie%2C+J+L">J. L. Conradie</a>, <a href="/search/nucl-ex?searchtype=author&query=Damache%2C+S">S. Damache</a>, <a href="/search/nucl-ex?searchtype=author&query=Debabi%2C+M">M. Debabi</a>, <a href="/search/nucl-ex?searchtype=author&query=Deloncle%2C+I">I. Deloncle</a>, <a href="/search/nucl-ex?searchtype=author&query=Easton%2C+J+L">J. L. Easton</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Jones%2C+P">P. Jones</a>, <a href="/search/nucl-ex?searchtype=author&query=Kheswa%2C+B+V">B. V. Kheswa</a>, <a href="/search/nucl-ex?searchtype=author&query=Khumalo%2C+N+A">N. A. Khumalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamula%2C+T">T. Lamula</a>, <a href="/search/nucl-ex?searchtype=author&query=Majola%2C+S+N+T">S. N. T. Majola</a>, <a href="/search/nucl-ex?searchtype=author&query=Ndayishimye%2C+J">J. Ndayishimye</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.07087v1-abstract-short" style="display: inline;"> Gamma-ray production cross section excitation functions have been measured for $30$, $42$, $54$ and $66$ MeV proton beams accelerated onto targets of astrophysical interest, $^{nat}$C, C + O (Mylar), $^{nat}$Mg, $^{nat}$Si and $^{56}$Fe, at the Sector Separated Cyclotron (SSC) of iThemba LABS (near Cape Town, South Africa). The AFRODITE array equipped with 8 Compton suppressed HPGe clover detector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.07087v1-abstract-full').style.display = 'inline'; document.getElementById('2001.07087v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.07087v1-abstract-full" style="display: none;"> Gamma-ray production cross section excitation functions have been measured for $30$, $42$, $54$ and $66$ MeV proton beams accelerated onto targets of astrophysical interest, $^{nat}$C, C + O (Mylar), $^{nat}$Mg, $^{nat}$Si and $^{56}$Fe, at the Sector Separated Cyclotron (SSC) of iThemba LABS (near Cape Town, South Africa). The AFRODITE array equipped with 8 Compton suppressed HPGe clover detectors was used to record $纬$-ray data. For known, intense $纬$-ray lines the previously reported experimental data measured up to $E_{p}\simeq$ $25$ MeV at the Washington and Orsay tandem accelerators were extended to higher proton energies. Our experimental data for the last 3 targets are reported here and discussed with respect to previous data and the Murphy \textit{et al.} compilation [ApJS 183, 142 (2009)], as well as to predictions of the nuclear reaction code TALYS. The overall agreement between theory and experiment obtained in first-approach calculations using default input parameters of TALYS has been appreciably improved by using modified optical model potential (OMP), deformation, and level density parameters. The OMP parameters have been extracted from theoretical fits to available experimental elastic/inelastic nucleon scattering angular distribution data by means of the coupled-channels reaction code OPTMAN. Experimental data for several new $纬$-ray lines are also reported and discussed. The astrophysical implications of our results are emphasised. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.07087v1-abstract-full').style.display = 'none'; document.getElementById('2001.07087v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 10 figures, five tables; regular article submitted to Phys Rev C</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 102, 025802 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.03600">arXiv:2001.03600</a> <span> [<a href="https://arxiv.org/pdf/2001.03600">pdf</a>, <a href="https://arxiv.org/format/2001.03600">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/1555/1/012011">10.1088/1742-6596/1555/1/012011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gamma-ray emission in alpha-particle reactions with C, Mg, Si, Fe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Bundesmann%2C+J">J. Bundesmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Deloncle%2C+I">I. Deloncle</a>, <a href="/search/nucl-ex?searchtype=author&query=Denker%2C+A">A. Denker</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Gostojic%2C+A">A. Gostojic</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6hrich%2C+J">J. R枚hrich</a>, <a href="/search/nucl-ex?searchtype=author&query=Benhabiles%2C+H">H. Benhabiles</a>, <a href="/search/nucl-ex?searchtype=author&query=Bougaoub%2C+I">I. Bougaoub</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Peyr%C3%A9%2C+J">J. Peyr茅</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.03600v1-abstract-short" style="display: inline;"> Cross sections for the strongest gamma-ray emission lines produced in alpha-particle reactions with C, Mg, Si, Fe have been measured in the range E_alpha = 50 - 90 MeV at the center for proton therapy at the Helmholtz-Zentrum Berlin. Data for more than 60 different gamma-ray lines were determined, with particular efforts for lines that are in cross section compilations/evaluations with astrophysic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03600v1-abstract-full').style.display = 'inline'; document.getElementById('2001.03600v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.03600v1-abstract-full" style="display: none;"> Cross sections for the strongest gamma-ray emission lines produced in alpha-particle reactions with C, Mg, Si, Fe have been measured in the range E_alpha = 50 - 90 MeV at the center for proton therapy at the Helmholtz-Zentrum Berlin. Data for more than 60 different gamma-ray lines were determined, with particular efforts for lines that are in cross section compilations/evaluations with astrophysical purpose, and where data exist at lower projectile energies. The data are compared with predictions of a modern nuclear reaction code and cross-section curves of the latest evaluation for gamma-ray line emission in accelerated-particle interactions in solar flares. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.03600v1-abstract-full').style.display = 'none'; document.getElementById('2001.03600v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 5 figures, contribution to the XXIII International School on Nuclear Physics, Neutron Physics and Applications, Varna, Bulgaria, September 22-28, 2019</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.04357">arXiv:1809.04357</a> <span> [<a href="https://arxiv.org/pdf/1809.04357">pdf</a>, <a href="https://arxiv.org/format/1809.04357">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/978-3-030-13876-9_45">10.1007/978-3-030-13876-9_45 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Charged-particle decays of highly excited states in $^{19}$F </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Chabot%2C+M">M. Chabot</a>, <a href="/search/nucl-ex?searchtype=author&query=Degerlier%2C+M">M. Degerlier</a>, <a href="/search/nucl-ex?searchtype=author&query=Delafosse%2C+C">C. Delafosse</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Georgiadou%2C+A">A. Georgiadou</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimar%C3%A3es%2C+V">V. Guimar茫es</a>, <a href="/search/nucl-ex?searchtype=author&query=Gottardo%2C+A">A. Gottardo</a>, <a href="/search/nucl-ex?searchtype=author&query=Matea%2C+I">I. Matea</a>, <a href="/search/nucl-ex?searchtype=author&query=Olivier%2C+L">L. Olivier</a>, <a href="/search/nucl-ex?searchtype=author&query=Perrot%2C+L">L. Perrot</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A">A. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Garg%2C+R">R. Garg</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillespie%2C+S">S. Gillespie</a>, <a href="/search/nucl-ex?searchtype=author&query=Riley%2C+J">J. Riley</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.04357v1-abstract-short" style="display: inline;"> Neutron-capture reactions on $^{18}$F in the helium-burning shell play an important role in the production of $^{15}$N during core-collapse supernovae. The competition between the $^{18}$F($n,p/伪$)$^{18}$O/$^{15}$N reactions controls the amount of $^{15}$N produced. The strengths of these reactions depend on the decay branching ratios of states in $^{19}$F above the neutron threshold. We report on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.04357v1-abstract-full').style.display = 'inline'; document.getElementById('1809.04357v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.04357v1-abstract-full" style="display: none;"> Neutron-capture reactions on $^{18}$F in the helium-burning shell play an important role in the production of $^{15}$N during core-collapse supernovae. The competition between the $^{18}$F($n,p/伪$)$^{18}$O/$^{15}$N reactions controls the amount of $^{15}$N produced. The strengths of these reactions depend on the decay branching ratios of states in $^{19}$F above the neutron threshold. We report on an experiment investigating the decay branching ratios of these states in order to better constrain the strengths of the reactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.04357v1-abstract-full').style.display = 'none'; document.getElementById('1809.04357v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted as part of the Proceedings of NIC 2018</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.00693">arXiv:1802.00693</a> <span> [<a href="https://arxiv.org/pdf/1802.00693">pdf</a>, <a href="https://arxiv.org/format/1802.00693">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.97.045807">10.1103/PhysRevC.97.045807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-resolution study of levels in the astrophysically important nucleus $^{26}$Mg and resulting updated level assignments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Br%C3%BCmmer%2C+J+W">J. W. Br眉mmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Meyer%2C+A">A. Meyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Neveling%2C+R">R. Neveling</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.00693v3-abstract-short" style="display: inline;"> The $^{22}$Ne($伪,n$)$^{25}$Mg reaction is an important source of neutrons for the s-process. Due to the difficulty in directly measuring the cross section of this reaction and the competing $^{22}$Ne($伪,纬$)$^{26}$Mg reaction, indirect methods are frequently used to try to instead calculate the relevant reaction rates. Uncertainty, however, persists in the number and properties of the pertinent exc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.00693v3-abstract-full').style.display = 'inline'; document.getElementById('1802.00693v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.00693v3-abstract-full" style="display: none;"> The $^{22}$Ne($伪,n$)$^{25}$Mg reaction is an important source of neutrons for the s-process. Due to the difficulty in directly measuring the cross section of this reaction and the competing $^{22}$Ne($伪,纬$)$^{26}$Mg reaction, indirect methods are frequently used to try to instead calculate the relevant reaction rates. Uncertainty, however, persists in the number and properties of the pertinent excited states of $^{26}$Mg. In this paper, the results of proton and deuteron scattering from $^{26}$Mg are presented, giving a list of levels in $^{26}$Mg. In addition, level assignments in $^{26}$Mg are discussed, including some possible changes to the previously accepted assignments in $^{26}$Mg. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.00693v3-abstract-full').style.display = 'none'; document.getElementById('1802.00693v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 3 figures, 2 tables. Fixed missing reference and some index labelling in figures, fixed page break problem under table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 97, 045807 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.05107">arXiv:1611.05107</a> <span> [<a href="https://arxiv.org/pdf/1611.05107">pdf</a>, <a href="https://arxiv.org/format/1611.05107">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.94.054314">10.1103/PhysRevC.94.054314 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Rearrangement of valence neutrons in the neutrinoless double-$尾$ decay of $^{136}$Xe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Szwec%2C+S+V">S. V. Szwec</a>, <a href="/search/nucl-ex?searchtype=author&query=Kay%2C+B+P">B. P. Kay</a>, <a href="/search/nucl-ex?searchtype=author&query=Cocolios%2C+T+E">T. E. Cocolios</a>, <a href="/search/nucl-ex?searchtype=author&query=Entwisle%2C+J+P">J. P. Entwisle</a>, <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+S+J">S. J. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaffney%2C+L+P">L. P. Gaffney</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimar%C3%A3es%2C+V">V. Guimar茫es</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=McKee%2C+P+P">P. P. McKee</a>, <a href="/search/nucl-ex?searchtype=author&query=Parr%2C+E">E. Parr</a>, <a href="/search/nucl-ex?searchtype=author&query=Portail%2C+C">C. Portail</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiffer%2C+J+P">J. P. Schiffer</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Sharp%2C+D+K">D. K. Sharp</a>, <a href="/search/nucl-ex?searchtype=author&query=Smith%2C+J+F">J. F. Smith</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.05107v1-abstract-short" style="display: inline;"> A quantitative description of the change in ground-state neutron occupancies between $^{136}$Xe and $^{136}$Ba, the initial and final state in the neutrinoless double-$尾$ decay of $^{136}$Xe, has been extracted from precision measurements of the cross sections of single-neutron adding and -removing reactions. Comparisons are made to recent theoretical calculations of the same properties using vari… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05107v1-abstract-full').style.display = 'inline'; document.getElementById('1611.05107v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.05107v1-abstract-full" style="display: none;"> A quantitative description of the change in ground-state neutron occupancies between $^{136}$Xe and $^{136}$Ba, the initial and final state in the neutrinoless double-$尾$ decay of $^{136}$Xe, has been extracted from precision measurements of the cross sections of single-neutron adding and -removing reactions. Comparisons are made to recent theoretical calculations of the same properties using various nuclear-structure models. These are the same calculations used to determine the magnitude of the nuclear matrix elements for the process, which at present disagree with each other by factors of 2 or 3. The experimental neutron occupancies show some disagreement with the theoretical calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05107v1-abstract-full').style.display = 'none'; document.getElementById('1611.05107v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 94, 054314 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.07810">arXiv:1605.07810</a> <span> [<a href="https://arxiv.org/pdf/1605.07810">pdf</a>, <a href="https://arxiv.org/ps/1605.07810">ps</a>, <a href="https://arxiv.org/format/1605.07810">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/i2015-15034-y">10.1140/epja/i2015-15034-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Recent results in nuclear astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">Alain Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">Fairouz Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">Juergen Kiener</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1605.07810v1-abstract-short" style="display: inline;"> In this review, we emphasize the interplay between astrophysical observations, modeling, and nuclear physics laboratory experiments. Several important nuclear cross sections for astrophysics have long been identified e.g. 12C(alpha,gamma)16O for stellar evolution, or 13C(alpha,n)16O and 22Ne(alpha,n)25Mg as neutron sources for the s-process. More recently, observations of lithium abundances in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.07810v1-abstract-full').style.display = 'inline'; document.getElementById('1605.07810v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.07810v1-abstract-full" style="display: none;"> In this review, we emphasize the interplay between astrophysical observations, modeling, and nuclear physics laboratory experiments. Several important nuclear cross sections for astrophysics have long been identified e.g. 12C(alpha,gamma)16O for stellar evolution, or 13C(alpha,n)16O and 22Ne(alpha,n)25Mg as neutron sources for the s-process. More recently, observations of lithium abundances in the oldest stars, or of nuclear gamma-ray lines from space, have required new laboratory experiments. New evaluation of thermonuclear reaction rates now includes the associated rate uncertainties that are used in astrophysical models to i) estimate final uncertainties on nucleosynthesis yields and ii) identify those reactions that require further experimental investigation. Sometimes direct cross section measurements are possible, but more generally the use of indirect methods is compulsory in view of the very low cross sections. Non-thermal processes are often overlooked but are also important for nuclear astrophysics, e.g. in gamma-ray emission from solar flares or in the interaction of cosmic rays with matter, and also motivate laboratory experiments. Finally, we show that beyond the historical motivations of nuclear astrophysics, understanding i) the energy sources that drive stellar evolution and ii) the origin of the elements can also be used to give new insights into physics beyond the standard model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.07810v1-abstract-full').style.display = 'none'; document.getElementById('1605.07810v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 33 Figures, invited review</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. A (2015) 51: 34 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.00305">arXiv:1512.00305</a> <span> [<a href="https://arxiv.org/pdf/1512.00305">pdf</a>, <a href="https://arxiv.org/ps/1512.00305">ps</a>, <a href="https://arxiv.org/format/1512.00305">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nima.2015.07.022">10.1016/j.nima.2015.07.022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fast-neutron induced background in LaBr3:Ce detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Deloncle%2C+I">I. Deloncle</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Laurent%2C+P">P. Laurent</a>, <a href="/search/nucl-ex?searchtype=author&query=Blondel%2C+C">C. Blondel</a>, <a href="/search/nucl-ex?searchtype=author&query=Chabot%2C+M">M. Chabot</a>, <a href="/search/nucl-ex?searchtype=author&query=Chipaux%2C+R">R. Chipaux</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Dubos%2C+S">S. Dubos</a>, <a href="/search/nucl-ex?searchtype=author&query=Gostojic%2C+A">A. Gostojic</a>, <a href="/search/nucl-ex?searchtype=author&query=Goutev%2C+N">N. Goutev</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Horeau%2C+B">B. Horeau</a>, <a href="/search/nucl-ex?searchtype=author&query=Limousin%2C+O">O. Limousin</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Pr%C3%A9vot%2C+G">G. Pr茅vot</a>, <a href="/search/nucl-ex?searchtype=author&query=Rodr%C3%ADguez-Gas%C3%A9n%2C+R">R. Rodr铆guez-Gas茅n</a>, <a href="/search/nucl-ex?searchtype=author&query=Yavahchova%2C+M+S">M. S. Yavahchova</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1512.00305v1-abstract-short" style="display: inline;"> The response of a scintillation detector with a cylindrical 1.5-inch LaBr3:Ce crystal to incident neutrons has been measured in the energy range En = 2-12 MeV. Neutrons were produced by proton irradiation of a Li target at Ep = 5-14.6 MeV with pulsed proton beams. Using the time-of-flight information between target and detector, energy spectra of the LaBr3:Ce detector resulting from fast neutron i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.00305v1-abstract-full').style.display = 'inline'; document.getElementById('1512.00305v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.00305v1-abstract-full" style="display: none;"> The response of a scintillation detector with a cylindrical 1.5-inch LaBr3:Ce crystal to incident neutrons has been measured in the energy range En = 2-12 MeV. Neutrons were produced by proton irradiation of a Li target at Ep = 5-14.6 MeV with pulsed proton beams. Using the time-of-flight information between target and detector, energy spectra of the LaBr3:Ce detector resulting from fast neutron interactions have been obtained at 4 different neutron energies. Neutron-induced gamma rays emitted by the LaBr3:Ce crystal were also measured in a nearby Ge detector at the lowest proton beam energy. In addition, we obtained data for neutron irradiation of a large-volume high-purity Ge detector and of a NE-213 liquid scintillator detector, both serving as monitor detectors in the experiment. Monte-Carlo type simulations for neutron interactions in the liquid scintillator, the Ge and LaBr3:Ce crystals have been performed and compared with measured data. Good agreement being obtained with the data, we present the results of simulations to predict the response of LaBr3:Ce detectors for a range of crystal sizes to neutron irradiation in the energy range En = 0.5-10 MeV <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.00305v1-abstract-full').style.display = 'none'; document.getElementById('1512.00305v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 10 figures, 4 Tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Instr. and Meth. in Physics Research A 798, 152 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00901">arXiv:1511.00901</a> <span> [<a href="https://arxiv.org/pdf/1511.00901">pdf</a>, <a href="https://arxiv.org/ps/1511.00901">ps</a>, <a href="https://arxiv.org/format/1511.00901">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.92.055806">10.1103/PhysRevC.92.055806 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopy of $^{19}$Ne for the thermonuclear $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reaction rates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulton%2C+B+R">B. R. Fulton</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1511.00901v1-abstract-short" style="display: inline;"> Uncertainties in the thermonuclear rates of the $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reactions affect model predictions of light curves from type I X-ray bursts and the amount of the observable radioisotope $^{18}$F produced in classical novae, respectively. To address these uncertainties, we have studied the nuclear structure of $^{19}$Ne over $E_{x} = 4.0 - 5.1$ MeV and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00901v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00901v1-abstract-full" style="display: none;"> Uncertainties in the thermonuclear rates of the $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reactions affect model predictions of light curves from type I X-ray bursts and the amount of the observable radioisotope $^{18}$F produced in classical novae, respectively. To address these uncertainties, we have studied the nuclear structure of $^{19}$Ne over $E_{x} = 4.0 - 5.1$ MeV and $6.1 - 7.3$ MeV using the $^{19}$F($^{3}$He,t)$^{19}$Ne reaction. We find the $J^蟺$ values of the 4.14 and 4.20 MeV levels to be consistent with $9/2^{-}$ and $7/2^{-}$ respectively, in contrast to previous assumptions. We confirm the recently observed triplet of states around 6.4 MeV, and find evidence that the state at 6.29 MeV, just below the proton threshold, is either broad or a doublet. Our data also suggest that predicted but yet unobserved levels may exist near the 6.86 MeV state. Higher resolution experiments are urgently needed to further clarify the structure of $^{19}$Ne around the proton threshold before a reliable $^{18}$F($p,伪$)$^{15}$O rate for nova models can be determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00901v1-abstract-full').style.display = 'none'; document.getElementById('1511.00901v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, Phys. Rev. C (in press)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.02656">arXiv:1507.02656</a> <span> [<a href="https://arxiv.org/pdf/1507.02656">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Gamma ray production cross sections in proton induced reactions on natural Mg, Si and Fe targets over the proton energy range 30 up to 66 MeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Yahia-Ch%C3%A9rif%2C+W">W. Yahia-Ch茅rif</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+E">E. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Lawrie%2C+J+J">J. J. Lawrie</a>, <a href="/search/nucl-ex?searchtype=author&query=Belhout%2C+A">A. Belhout</a>, <a href="/search/nucl-ex?searchtype=author&query=Benhabiles%2C+H">H. Benhabiles</a>, <a href="/search/nucl-ex?searchtype=author&query=Bucher%2C+T+D">T. D. Bucher</a>, <a href="/search/nucl-ex?searchtype=author&query=Chafa%2C+A">A. Chafa</a>, <a href="/search/nucl-ex?searchtype=author&query=Damache%2C+S">S. Damache</a>, <a href="/search/nucl-ex?searchtype=author&query=Debabi%2C+M">M. Debabi</a>, <a href="/search/nucl-ex?searchtype=author&query=Deloncle%2C+I">I. Deloncle</a>, <a href="/search/nucl-ex?searchtype=author&query=Easton%2C+J+L">J. L. Easton</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Jones%2C+P">P. Jones</a>, <a href="/search/nucl-ex?searchtype=author&query=Kheswa%2C+B+V">B. V. Kheswa</a>, <a href="/search/nucl-ex?searchtype=author&query=Khumalo%2C+N">N. Khumalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamula%2C+T">T. Lamula</a>, <a href="/search/nucl-ex?searchtype=author&query=Majola%2C+S+T+H">S. T. H. Majola</a>, <a href="/search/nucl-ex?searchtype=author&query=Negi%2C+D">D. Negi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ndayishimye%2C+J">J. Ndayishimye</a>, <a href="/search/nucl-ex?searchtype=author&query=Noncolela%2C+S+P">S. P. Noncolela</a>, <a href="/search/nucl-ex?searchtype=author&query=Moussa%2C+D">D. Moussa</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.02656v1-abstract-short" style="display: inline;"> Gamma-ray excitation functions have been measured for 30, 42, 54 and 66 MeV proton beams accelerated onto C + O (Mylar), Mg, Si, and Fe targets of astrophysical interest at the separate-sector cyclotron of iThemba LABS in Somerset West (Cape Town, South Africa). A large solid angle, high energy resolution detection system of the Eurogam type was used to record Gamma-ray energy spectra. Derived pre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02656v1-abstract-full').style.display = 'inline'; document.getElementById('1507.02656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.02656v1-abstract-full" style="display: none;"> Gamma-ray excitation functions have been measured for 30, 42, 54 and 66 MeV proton beams accelerated onto C + O (Mylar), Mg, Si, and Fe targets of astrophysical interest at the separate-sector cyclotron of iThemba LABS in Somerset West (Cape Town, South Africa). A large solid angle, high energy resolution detection system of the Eurogam type was used to record Gamma-ray energy spectra. Derived preliminary results of Gamma-ray line production cross sections for the Mg, Si and Fe target nuclei are reported and discussed. The current cross section data for known, intense Gamma-ray lines from these nuclei consistently extend to higher proton energies previous experimental data measured up to Ep ~ 25 MeV at the Orsay and Washington tandem accelerators. Data for new Gamma-ray lines observed for the first time in this work are also reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.02656v1-abstract-full').style.display = 'none'; document.getElementById('1507.02656v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures. IOP Institute of Physics Conference Nuclear Physics in Astrophysics VII, 28th EPF Nuclear Physics Divisional Conference, May 18-22 2015, York, UK</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.00593">arXiv:1505.00593</a> <span> [<a href="https://arxiv.org/pdf/1505.00593">pdf</a>, <a href="https://arxiv.org/ps/1505.00593">ps</a>, <a href="https://arxiv.org/format/1505.00593">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.92.015805">10.1103/PhysRevC.92.015805 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First application of the Trojan Horse Method with a Radioactive Ion Beam: study of the $^{18}$F($p,伪$)$^{15}$O}} reaction at astrophysical energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Gulino%2C+M">M. Gulino</a>, <a href="/search/nucl-ex?searchtype=author&query=Spitaleri%2C+C">C. Spitaleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapisarda%2C+G+G">G. G. Rapisarda</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L. Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Pizzone%2C+R+G">R. G. Pizzone</a>, <a href="/search/nucl-ex?searchtype=author&query=Romano%2C+S">S. Romano</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">S. Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kato%2C+S">S. Kato</a>, <a href="/search/nucl-ex?searchtype=author&query=Komatsubara%2C+T">T. Komatsubara</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiss%2C+G">G. Kiss</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishop%2C+S">S. Bishop</a>, <a href="/search/nucl-ex?searchtype=author&query=Binh%2C+D+N">D. N. Binh</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1505.00593v1-abstract-short" style="display: inline;"> Measurement of nuclear cross sections at astrophysical energies involving unstable species is one of the most challenging tasks in experimental nuclear physics. The use of indirect methods is often unavoidable in this scenario. In this paper the Trojan Horse Method is applied for the first time to a radioactive ion beam induced reaction studying the $^{18}$F($p,伪$)$^{15}$O process at low energies… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.00593v1-abstract-full').style.display = 'inline'; document.getElementById('1505.00593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.00593v1-abstract-full" style="display: none;"> Measurement of nuclear cross sections at astrophysical energies involving unstable species is one of the most challenging tasks in experimental nuclear physics. The use of indirect methods is often unavoidable in this scenario. In this paper the Trojan Horse Method is applied for the first time to a radioactive ion beam induced reaction studying the $^{18}$F($p,伪$)$^{15}$O process at low energies relevant to astrophysics via the three body reaction $^{2}$H($^{18}$F,$伪^{15}$O)n. The knowledge of the $^{18}$F($p, 伪$)$^{15}$O reaction rate is crucial to understand the nova explosion phenomena. The cross section of this reaction is characterized by the presence of several resonances in $^{19}$Ne and possibly interference effects among them. The results reported in Literature are not satisfactory and new investigations of the $^{18}$F($p,伪$)$^{15}$O reaction cross section will be useful. In the present work the spin-parity assignments of relevant levels have been discussed and the astrophysical S-factor has been extracted considering also interference effects <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.00593v1-abstract-full').style.display = 'none'; document.getElementById('1505.00593v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.1593">arXiv:1401.1593</a> <span> [<a href="https://arxiv.org/pdf/1401.1593">pdf</a>, <a href="https://arxiv.org/format/1401.1593">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.112.042502">10.1103/PhysRevLett.112.042502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental study of the two-body spin-orbit force </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Burgunder%2C+G">G. Burgunder</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Nowacki%2C+F">F. Nowacki</a>, <a href="/search/nucl-ex?searchtype=author&query=Giron%2C+S">S. Giron</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Moukaddam%2C+M">M. Moukaddam</a>, <a href="/search/nucl-ex?searchtype=author&query=eville%2C+N+D+S+e">N. De S er eville</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=aceres%2C+L+C">L. C aceres</a>, <a href="/search/nucl-ex?searchtype=author&query=%C3%A9ment%2C+E+C">E. Cl 茅ment</a>, <a href="/search/nucl-ex?searchtype=author&query=Duch%C3%AAne%2C+G">G. Duch锚ne</a>, <a href="/search/nucl-ex?searchtype=author&query=Ebran%2C+J+P">J. P. Ebran</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Flavigny%2C+F">F. Flavigny</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Gibelin%2C+J">J. Gibelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillibert%2C+A">A. Gillibert</a>, <a href="/search/nucl-ex?searchtype=author&query=%C3%A9vy%2C+S+G">S. Gr 茅vy</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Lepailleur%2C+A">A. Lepailleur</a>, <a href="/search/nucl-ex?searchtype=author&query=Matea%2C+I">I. Matea</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Nalpas%2C+L">L. Nalpas</a>, <a href="/search/nucl-ex?searchtype=author&query=Obertelli%2C+A">A. Obertelli</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1401.1593v1-abstract-short" style="display: inline;"> Energies and spectroscopic factors of the first $7/2^-$, $3/2^-$, $1/2^-$ and $5/2^-$ states in the $^{35}$Si$_{21}$ nucleus were determined by means of the (d,p) transfer reaction in inverse kinematics at GANIL using the MUST2 and EXOGAM detectors. By comparing the spectroscopic information on the $^{35}$Si and $^{37}$S isotones, a reduction of the $p_{3/2} - p_{1/2}$ spin-orbit splitting by abou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1593v1-abstract-full').style.display = 'inline'; document.getElementById('1401.1593v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.1593v1-abstract-full" style="display: none;"> Energies and spectroscopic factors of the first $7/2^-$, $3/2^-$, $1/2^-$ and $5/2^-$ states in the $^{35}$Si$_{21}$ nucleus were determined by means of the (d,p) transfer reaction in inverse kinematics at GANIL using the MUST2 and EXOGAM detectors. By comparing the spectroscopic information on the $^{35}$Si and $^{37}$S isotones, a reduction of the $p_{3/2} - p_{1/2}$ spin-orbit splitting by about 25% is proposed, while the $f_{7/2} -f_{5/2}$ spin-orbit splitting seems to remain constant. These features, derived after having unfolded nuclear correlations using shell model calculations, have been attributed to the properties of the 2-body spin-orbit interaction, the amplitude of which is derived for the first time in an atomic nucleus. The present results, remarkably well reproduced by using several realistic nucleon-nucleon forces, provide a unique touchstone for the modeling of the spin-orbit interaction in atomic nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1593v1-abstract-full').style.display = 'none'; document.getElementById('1401.1593v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, accepted for publication in Physical Review Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.0894">arXiv:1312.0894</a> <span> [<a href="https://arxiv.org/pdf/1312.0894">pdf</a>, <a href="https://arxiv.org/ps/1312.0894">ps</a>, <a href="https://arxiv.org/format/1312.0894">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.88.062802">10.1103/PhysRevC.88.062802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for new resonant states in 10C and 11C and their impact on the cosmological lithium problem </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Roussel%2C+P">P. Roussel</a>, <a href="/search/nucl-ex?searchtype=author&query=Ancelin%2C+S">S. Ancelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Audouin%2C+L">L. Audouin</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S">S. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A">A. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Crom%2C+B+L">B. Le Crom</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre%2C+L">L. Lefebvre</a>, <a href="/search/nucl-ex?searchtype=author&query=Matea%2C+I">I. Matea</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Mavilla%2C+G">G. Mavilla</a>, <a href="/search/nucl-ex?searchtype=author&query=Mrazek%2C+J">J. Mrazek</a>, <a href="/search/nucl-ex?searchtype=author&query=Morfouace%2C+P">P. Morfouace</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1312.0894v1-abstract-short" style="display: inline;"> The observed primordial 7Li abundance in metal-poor halo stars is found to be lower than its Big-Bang nucleosynthesis (BBN) calculated value by a factor of approximately three. Some recent works suggested the possibility that this discrepancy originates from missing resonant reactions which would destroy the 7Be, parent of 7Li. The most promising candidate resonances which were found include a pos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0894v1-abstract-full').style.display = 'inline'; document.getElementById('1312.0894v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.0894v1-abstract-full" style="display: none;"> The observed primordial 7Li abundance in metal-poor halo stars is found to be lower than its Big-Bang nucleosynthesis (BBN) calculated value by a factor of approximately three. Some recent works suggested the possibility that this discrepancy originates from missing resonant reactions which would destroy the 7Be, parent of 7Li. The most promising candidate resonances which were found include a possibly missed 1- or 2- narrow state around 15 MeV in the compound nucleus 10C formed by 7Be+3He and a state close to 7.8 MeV in the compound nucleus 11C formed by 7Be+4He. In this work, we studied the high excitation energy region of 10C and the low excitation energy region in 11C via the reactions 10B(3He,t)10C and 11B(3He,t)11C, respectively, at the incident energy of 35 MeV. Our results for 10C do not support 7Be+3He as a possible solution for the 7Li problem. Concerning 11C results, the data show no new resonances in the excitation energy region of interest and this excludes 7Be+4He reaction channel as an explanation for the 7Li deficit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0894v1-abstract-full').style.display = 'none'; document.getElementById('1312.0894v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Phys. Rev. C (Rapid Communication)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.1632">arXiv:1310.1632</a> <span> [<a href="https://arxiv.org/pdf/1310.1632">pdf</a>, <a href="https://arxiv.org/format/1310.1632">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/665/1/012044">10.1088/1742-6596/665/1/012044 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nuclear astrophysics with radioactive ions at FAIR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Reifarth%2C+R">R. Reifarth</a>, <a href="/search/nucl-ex?searchtype=author&query=Altstadt%2C+S">S. Altstadt</a>, <a href="/search/nucl-ex?searchtype=author&query=G%C3%B6bel%2C+K">K. G枚bel</a>, <a href="/search/nucl-ex?searchtype=author&query=Heftrich%2C+T">T. Heftrich</a>, <a href="/search/nucl-ex?searchtype=author&query=Heil%2C+M">M. Heil</a>, <a href="/search/nucl-ex?searchtype=author&query=Koloczek%2C+A">A. Koloczek</a>, <a href="/search/nucl-ex?searchtype=author&query=Langer%2C+C">C. Langer</a>, <a href="/search/nucl-ex?searchtype=author&query=Plag%2C+R">R. Plag</a>, <a href="/search/nucl-ex?searchtype=author&query=Pohl%2C+M">M. Pohl</a>, <a href="/search/nucl-ex?searchtype=author&query=Sonnabend%2C+K">K. Sonnabend</a>, <a href="/search/nucl-ex?searchtype=author&query=Weigand%2C+M">M. Weigand</a>, <a href="/search/nucl-ex?searchtype=author&query=Adachi%2C+T">T. Adachi</a>, <a href="/search/nucl-ex?searchtype=author&query=Aksouh%2C+F">F. Aksouh</a>, <a href="/search/nucl-ex?searchtype=author&query=Al-Khalili%2C+J">J. Al-Khalili</a>, <a href="/search/nucl-ex?searchtype=author&query=AlGarawi%2C+M">M. AlGarawi</a>, <a href="/search/nucl-ex?searchtype=author&query=AlGhamdi%2C+S">S. AlGhamdi</a>, <a href="/search/nucl-ex?searchtype=author&query=Alkhazov%2C+G">G. Alkhazov</a>, <a href="/search/nucl-ex?searchtype=author&query=Alkhomashi%2C+N">N. Alkhomashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez-Pol%2C+H">H. Alvarez-Pol</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez-Rodriguez%2C+R">R. Alvarez-Rodriguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Andreev%2C+V">V. Andreev</a>, <a href="/search/nucl-ex?searchtype=author&query=Andrei%2C+B">B. Andrei</a>, <a href="/search/nucl-ex?searchtype=author&query=Atar%2C+L">L. Atar</a>, <a href="/search/nucl-ex?searchtype=author&query=Aumann%2C+T">T. Aumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Avdeichikov%2C+V">V. Avdeichikov</a> , et al. (295 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1310.1632v1-abstract-short" style="display: inline;"> The nucleosynthesis of elements beyond iron is dominated by neutron captures in the s and r processes. However, 32 stable, proton-rich isotopes cannot be formed during those processes, because they are shielded from the s-process flow and r-process beta-decay chains. These nuclei are attributed to the p and rp process. For all those processes, current research in nuclear astrophysics addresses t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1632v1-abstract-full').style.display = 'inline'; document.getElementById('1310.1632v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.1632v1-abstract-full" style="display: none;"> The nucleosynthesis of elements beyond iron is dominated by neutron captures in the s and r processes. However, 32 stable, proton-rich isotopes cannot be formed during those processes, because they are shielded from the s-process flow and r-process beta-decay chains. These nuclei are attributed to the p and rp process. For all those processes, current research in nuclear astrophysics addresses the need for more precise reaction data involving radioactive isotopes. Depending on the particular reaction, direct or inverse kinematics, forward or time-reversed direction are investigated to determine or at least to constrain the desired reaction cross sections. The Facility for Antiproton and Ion Research (FAIR) will offer unique, unprecedented opportunities to investigate many of the important reactions. The high yield of radioactive isotopes, even far away from the valley of stability, allows the investigation of isotopes involved in processes as exotic as the r or rp processes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.1632v1-abstract-full').style.display = 'none'; document.getElementById('1310.1632v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Invited Talk given at the Conference Nuclear Physice in Astrophysics VI (NPA6), Lisbon, Portugal, May 19-24 2013. To appear in the NPA6 Proceedings in Journal of Physics: Conference Series (JPCS)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics: Conference Series 665 (2016) 012044 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1210.8269">arXiv:1210.8269</a> <span> [<a href="https://arxiv.org/pdf/1210.8269">pdf</a>, <a href="https://arxiv.org/ps/1210.8269">ps</a>, <a href="https://arxiv.org/format/1210.8269">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/420/1/012149">10.1088/1742-6596/420/1/012149 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trojan Horse method and radioactive ion beams: study of $^{18}$F(p,$伪$)$^{15}$O reaction at astrophysical energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Gulino%2C+M">M. Gulino</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapisarda%2C+G+G">G. G. Rapisarda</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L. Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">S. Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kato%2C+S">S. Kato</a>, <a href="/search/nucl-ex?searchtype=author&query=Komatsubara%2C+H">H. Komatsubara</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=De+S%C3%A9r%C3%A9ville%2C+N">N. De S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Spitaleri%2C+C">C. Spitaleri</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1210.8269v1-abstract-short" style="display: inline;"> The Trojan Horse Method was applied for the first time to a Radioactive Ion Beam induced reaction to study the reaction $^{18}$F(p,$伪$)$^{15}$O via the three body reaction $^{18}$F(d,$伪$ $^{15}$O)n at the low energies relevant for astrophysics. The abundance of $^{18}$F in Nova explosions is an important issue for the understanding of this astrophysical phenomenon. For this reason it is necessary… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.8269v1-abstract-full').style.display = 'inline'; document.getElementById('1210.8269v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1210.8269v1-abstract-full" style="display: none;"> The Trojan Horse Method was applied for the first time to a Radioactive Ion Beam induced reaction to study the reaction $^{18}$F(p,$伪$)$^{15}$O via the three body reaction $^{18}$F(d,$伪$ $^{15}$O)n at the low energies relevant for astrophysics. The abundance of $^{18}$F in Nova explosions is an important issue for the understanding of this astrophysical phenomenon. For this reason it is necessary to study the nuclear reactions that produce or destroy $^{18}$F in Novae. $^{18}$F(p,$伪$)$^{15}$O is one of the main $^{18}$F destruction channels. Preliminary results are presented in this paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.8269v1-abstract-full').style.display = 'none'; document.getElementById('1210.8269v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Talk given by Marisa Gulino at the 11th International Conference on Nucleus-Nucleus Collisions (NN2012), San Antonio, Texas, USA, May 27-June 1, 2012. To appear in the NN2012 Proceedings in Journal of Physics: Conference Series (JPCS)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1012.4040">arXiv:1012.4040</a> <span> [<a href="https://arxiv.org/pdf/1012.4040">pdf</a>, <a href="https://arxiv.org/ps/1012.4040">ps</a>, <a href="https://arxiv.org/format/1012.4040">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.84.011301">10.1103/PhysRevC.84.011301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.84.029902">10.1103/PhysRevC.84.029902 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Emergence of the N=16 shell gap in 21O </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Thomas%2C+J+S">J. S. Thomas</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W+N">W. N. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Delaunay%2C+F">F. Delaunay</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+S+M">S. M. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Orr%2C+N+A">N. A. Orr</a>, <a href="/search/nucl-ex?searchtype=author&query=Rejmund%2C+M">M. Rejmund</a>, <a href="/search/nucl-ex?searchtype=author&query=Achouri%2C+N+L">N. L. Achouri</a>, <a href="/search/nucl-ex?searchtype=author&query=Falou%2C+H+A">H. Al Falou</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashwood%2C+N+A">N. A. Ashwood</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Blumenfeld%2C+Y">Y. Blumenfeld</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Chapman%2C+R">R. Chapman</a>, <a href="/search/nucl-ex?searchtype=author&query=Chartier%2C+M">M. Chartier</a>, <a href="/search/nucl-ex?searchtype=author&query=Curtis%2C+N">N. Curtis</a>, <a href="/search/nucl-ex?searchtype=author&query=Force%2C+C">C. Force</a>, <a href="/search/nucl-ex?searchtype=author&query=de+France%2C+G">G. de France</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillot%2C+J">J. Guillot</a>, <a href="/search/nucl-ex?searchtype=author&query=Haigh%2C+P">P. Haigh</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Labiche%2C+M">M. Labiche</a>, <a href="/search/nucl-ex?searchtype=author&query=Lapoux%2C+V">V. Lapoux</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemmon%2C+R+C">R. C. Lemmon</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1012.4040v1-abstract-short" style="display: inline;"> The spectroscopy of 21O has been investigated using a radioactive 20O beam and the (d,p) reaction in inverse kinematics. The ground and first excited states have been determined to be Jpi=5/2+ and Jpi=1/2+ respectively. Two neutron unbound states were observed at excitation energies of 4.76 +- 0.10 and 6.16 +- 0.11. The spectroscopic factor deduced for the lower of these interpreted as a 3/2+ leve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.4040v1-abstract-full').style.display = 'inline'; document.getElementById('1012.4040v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1012.4040v1-abstract-full" style="display: none;"> The spectroscopy of 21O has been investigated using a radioactive 20O beam and the (d,p) reaction in inverse kinematics. The ground and first excited states have been determined to be Jpi=5/2+ and Jpi=1/2+ respectively. Two neutron unbound states were observed at excitation energies of 4.76 +- 0.10 and 6.16 +- 0.11. The spectroscopic factor deduced for the lower of these interpreted as a 3/2+ level, reveals a rather pure 0d3/2 single-particle configuration. The large energy difference between the 3/2+ and 1/2+ states is indicative of the emergence of the N=16 magic number. For the higher lying resonance, which has a character consistent with a spin-parity assignment of 3/2+ or 7/2-, a 71% branching ratio to the first 2+ state in 20O has been observed. The results are compared with new shell model calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1012.4040v1-abstract-full').style.display = 'none'; document.getElementById('1012.4040v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 December, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C84:011301,2011; Publisher-note C84:029902,2011; Phys.Rev.C84:029902,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1011.6179">arXiv:1011.6179</a> <span> [<a href="https://arxiv.org/pdf/1011.6179">pdf</a>, <a href="https://arxiv.org/ps/1011.6179">ps</a>, <a href="https://arxiv.org/format/1011.6179">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.82.065803">10.1103/PhysRevC.82.065803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-energy break-up of 6Li as a tool to study the Big-Bang nucleosynthesis reaction 2H(alpha,gamma)6Li </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Heil%2C+M">M. Heil</a>, <a href="/search/nucl-ex?searchtype=author&query=Typel%2C+S">S. Typel</a>, <a href="/search/nucl-ex?searchtype=author&query=Galaviz%2C+D">D. Galaviz</a>, <a href="/search/nucl-ex?searchtype=author&query=S%C3%BCmmerer%2C+K">K. S眉mmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Uhlig%2C+F">F. Uhlig</a>, <a href="/search/nucl-ex?searchtype=author&query=Attallah%2C+F">F. Attallah</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Cortina%2C+D">D. Cortina</a>, <a href="/search/nucl-ex?searchtype=author&query=Geissel%2C+H">H. Geissel</a>, <a href="/search/nucl-ex?searchtype=author&query=Hellstr%C3%B6m%2C+M">M. Hellstr枚m</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Koczon%2C+P">P. Koczon</a>, <a href="/search/nucl-ex?searchtype=author&query=Kohlmeyer%2C+B">B. Kohlmeyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Mohr%2C+P">P. Mohr</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwab%2C+E">E. Schwab</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwarz%2C+K">K. Schwarz</a>, <a href="/search/nucl-ex?searchtype=author&query=Sch%C3%BCmann%2C+F">F. Sch眉mann</a>, <a href="/search/nucl-ex?searchtype=author&query=Senger%2C+P">P. Senger</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Thibaud%2C+J+P">J. P. Thibaud</a>, <a href="/search/nucl-ex?searchtype=author&query=Vangioni%2C+E">E. Vangioni</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1011.6179v1-abstract-short" style="display: inline;"> The recently claimed observations of non-negligible amounts of 6Li in old halo stars have renewed interest in the Big-Bang Nucleosynthesis (BBN) of 6Li. One important ingredient in the predicted BBN abundance of 6Li is the low-energy 2H(alpha,gamma)6Li cross section. Up to now, the only available experimental result for this cross section showed an almost constant astrophysical S-factor below 400… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.6179v1-abstract-full').style.display = 'inline'; document.getElementById('1011.6179v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1011.6179v1-abstract-full" style="display: none;"> The recently claimed observations of non-negligible amounts of 6Li in old halo stars have renewed interest in the Big-Bang Nucleosynthesis (BBN) of 6Li. One important ingredient in the predicted BBN abundance of 6Li is the low-energy 2H(alpha,gamma)6Li cross section. Up to now, the only available experimental result for this cross section showed an almost constant astrophysical S-factor below 400 keV, contrary to theoretical expectations. We report on a new measurement of the 2H(alpha,gamma)6Li reaction using the break-up of 6Li at 150 A MeV. Even though we cannot separate experimentally the Coulomb contribution from the nuclear one, we find clear evidence for Coulomb-nuclear interference by analyzing the scattering-angular distributions. This is in-line with our theoretical description which indicates a drop of the S_24-factor at low energies as predicted also by most other models. Consequently, we find even lower upper limits for the calculated primordial 6Li abundance than before. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1011.6179v1-abstract-full').style.display = 'none'; document.getElementById('1011.6179v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 11 figures, LaTeX, submitted to Phy. Rev. C</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C82:065803,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0810.3890">arXiv:0810.3890</a> <span> [<a href="https://arxiv.org/pdf/0810.3890">pdf</a>, <a href="https://arxiv.org/ps/0810.3890">ps</a>, <a href="https://arxiv.org/format/0810.3890">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Rapid onset of collectivity in the vicinity of 78Ni </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Matthieu%2C+L">Lebois Matthieu</a>, <a href="/search/nucl-ex?searchtype=author&query=Verney%2C+D">David Verney</a>, <a href="/search/nucl-ex?searchtype=author&query=Ibrahim%2C+F">Fadi Ibrahim</a>, <a href="/search/nucl-ex?searchtype=author&query=Essabaa%2C+S">Said Essabaa</a>, <a href="/search/nucl-ex?searchtype=author&query=Azaiez%2C+F">Fai莽al Azaiez</a>, <a href="/search/nucl-ex?searchtype=author&query=Mhamed%2C+M+C">Maher Cheikh Mhamed</a>, <a href="/search/nucl-ex?searchtype=author&query=Cottereau%2C+E">Evelyne Cottereau</a>, <a href="/search/nucl-ex?searchtype=author&query=Viet%2C+C+P">Cuong Phan Viet</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraton%2C+M">Mathieu Ferraton</a>, <a href="/search/nucl-ex?searchtype=author&query=Flanagan%2C+K">Kieran Flanagan</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">Serge Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Mueller%2C+D+G">Dominique Guillemaud Mueller</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">Fairouz Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Lau%2C+C">Christophe Lau</a>, <a href="/search/nucl-ex?searchtype=author&query=Blanc%2C+F+L">Fran莽ois Le Blanc</a>, <a href="/search/nucl-ex?searchtype=author&query=Du%2C+J+F+L">Jean Fran莽ois Le Du</a>, <a href="/search/nucl-ex?searchtype=author&query=Mouginot%2C+B">Baptiste Mouginot</a>, <a href="/search/nucl-ex?searchtype=author&query=Petrache%2C+C">Costel Petrache</a>, <a href="/search/nucl-ex?searchtype=author&query=Roussi%C3%A8re%2C+B">Brigitte Roussi猫re</a>, <a href="/search/nucl-ex?searchtype=author&query=Sagui%2C+L">Lionel Sagui</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Sereville%2C+N">Nicolas De Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">Iulian Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Tastet%2C+B">Benoit Tastet</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0810.3890v1-abstract-short" style="display: inline;"> gamma-rays following the B and B-n decay of the very neutron rich 84Ga produced by photo-fission of 238U have been studied at the newly built ISOL facility of IPN Orsay: ALTO. Two activities were observed and assigned to two B-decaying states: 84gGa, I = (0\^-) and 84mGa, I = (3\^-, 4\^-). Excitation energies of the 2+1 and 4+1 excited states of 84Ge were measured at E(2+1) = 624.3 keV and E(4+1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.3890v1-abstract-full').style.display = 'inline'; document.getElementById('0810.3890v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0810.3890v1-abstract-full" style="display: none;"> gamma-rays following the B and B-n decay of the very neutron rich 84Ga produced by photo-fission of 238U have been studied at the newly built ISOL facility of IPN Orsay: ALTO. Two activities were observed and assigned to two B-decaying states: 84gGa, I = (0\^-) and 84mGa, I = (3\^-, 4\^-). Excitation energies of the 2+1 and 4+1 excited states of 84Ge were measured at E(2+1) = 624.3 keV and E(4+1) = 1670.1 keV. Comparison with HFB+GCM calculations allows to establish the collective character of this nucleus indicating a substantial N=50 core polarization. The excitation energy of the 1/2+1 state in 83Ga known to carry a large part of the neutron 3s1/2 strength was measured at 247.8keV. Altogether these data allow to confirm the new single particle state ordering which appears immediately after the double Z=28 and N=50 shell closure and to designate 78Ni as a fragile and easily polarized doubly-magic core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0810.3890v1-abstract-full').style.display = 'none'; document.getElementById('0810.3890v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 October, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, ReVTeX</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0702034">arXiv:nucl-ex/0702034</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0702034">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0702034">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0702034">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.nuclphysa.2007.02.003">10.1016/j.nuclphysa.2007.02.003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Indirect study of 19Ne states near the 18F+p threshold </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=de+Sereville%2C+N">N. de Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Angulo%2C+C">C. Angulo</a>, <a href="/search/nucl-ex?searchtype=author&query=Assuncao%2C+M">M. Assuncao</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=berthoumieux%2C+E">E. berthoumieux</a>, <a href="/search/nucl-ex?searchtype=author&query=Bouzid%2C+B">B. Bouzid</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Couder%2C+M">M. Couder</a>, <a href="/search/nucl-ex?searchtype=author&query=Demaret%2C+P">P. Demaret</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Figuera%2C+P">P. Figuera</a>, <a href="/search/nucl-ex?searchtype=author&query=Fortier%2C+S">S. Fortier</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaelens%2C+M">M. Gaelens</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Labar%2C+D">D. Labar</a>, <a href="/search/nucl-ex?searchtype=author&query=Leleux%2C+P">P. Leleux</a>, <a href="/search/nucl-ex?searchtype=author&query=Loiselet%2C+M">M. Loiselet</a>, <a href="/search/nucl-ex?searchtype=author&query=Ninane%2C+A">A. Ninane</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Ryckewaert%2C+G">G. Ryckewaert</a>, <a href="/search/nucl-ex?searchtype=author&query=Smirnova%2C+N">N. Smirnova</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0702034v1-abstract-short" style="display: inline;"> The early E < 511 keV gamma-ray emission from novae depends critically on the 18F(p,a)15O reaction. Unfortunately the reaction rate of the 18F(p,a)15O reaction is still largely uncertain due to the unknown strengths of low-lying proton resonances near the 18F+p threshold which play an important role in the nova temperature regime. We report here our last results concerning the study of the d(18F… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0702034v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0702034v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0702034v1-abstract-full" style="display: none;"> The early E < 511 keV gamma-ray emission from novae depends critically on the 18F(p,a)15O reaction. Unfortunately the reaction rate of the 18F(p,a)15O reaction is still largely uncertain due to the unknown strengths of low-lying proton resonances near the 18F+p threshold which play an important role in the nova temperature regime. We report here our last results concerning the study of the d(18F,p)19F(alpha)15N transfer reaction. We show in particular that these two low-lying resonances cannot be neglected. These results are then used to perform a careful study of the remaining uncertainties associated to the 18F(p,a)15O and 18F(p,g)19Ne reaction rates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0702034v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0702034v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 8 figures. Accepted in Nuclear Physics A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys.A791:251-266,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0701066">arXiv:nucl-ex/0701066</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0701066">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0701066">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0701066">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.76.054312">10.1103/PhysRevC.76.054312 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low Energy States of $^{81}_{31} Ga_{50}$ : Elements on the Doubly-Magic Nature of $^{78}$Ni </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Verney%2C+D">David Verney</a>, <a href="/search/nucl-ex?searchtype=author&query=Bourgeois%2C+C">C. Bourgeois</a>, <a href="/search/nucl-ex?searchtype=author&query=Donzaud%2C+C">C. Donzaud</a>, <a href="/search/nucl-ex?searchtype=author&query=Essabaa%2C+S">S. Essabaa</a>, <a href="/search/nucl-ex?searchtype=author&query=Gales%2C+S">S. Gales</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaudefroy%2C+L">L. Gaudefroy</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillemaud-Mueller%2C+D">D. Guillemaud-Mueller</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Ibrahim%2C+F">F. Ibrahim</a>, <a href="/search/nucl-ex?searchtype=author&query=Lau%2C+C">C. Lau</a>, <a href="/search/nucl-ex?searchtype=author&query=Blanc%2C+F+L">F. Le Blanc</a>, <a href="/search/nucl-ex?searchtype=author&query=Mueller%2C+A+C">A. C. Mueller</a>, <a href="/search/nucl-ex?searchtype=author&query=Perru%2C+O">O. Perru</a>, <a href="/search/nucl-ex?searchtype=author&query=Pougheon%2C+F">F. Pougheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Roussiere%2C+B">B. Roussiere</a>, <a href="/search/nucl-ex?searchtype=author&query=Sauvage%2C+J">J. Sauvage</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Verney%2C+D">D. Verney</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0701066v1-abstract-short" style="display: inline;"> Excited levels were attributed to $^{81}_{31}$Ga$_{50}$ for the first time which were fed in the $尾$-decay of its mother nucleus $^{81}$Zn produced in the fission of $^{nat}$U using the ISOL technique. We show that the structure of this nucleus is consistent with that of the less exotic proton-deficient N=50 isotones within the assumption of strong proton Z=28 and neutron N=50 effective shell ef… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0701066v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0701066v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0701066v1-abstract-full" style="display: none;"> Excited levels were attributed to $^{81}_{31}$Ga$_{50}$ for the first time which were fed in the $尾$-decay of its mother nucleus $^{81}$Zn produced in the fission of $^{nat}$U using the ISOL technique. We show that the structure of this nucleus is consistent with that of the less exotic proton-deficient N=50 isotones within the assumption of strong proton Z=28 and neutron N=50 effective shell effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0701066v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0701066v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, REVTeX 4, 5 figures (eps format)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C76:054312,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0612001">arXiv:nucl-ex/0612001</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0612001">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0612001">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0612001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.75.044603">10.1103/PhysRevC.75.044603 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spallation Residues in the Reaction 56Fe + p at 0.3, 0.5, 0.75, 1.0 and 1.5 A GeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Villagrasa-Canton%2C+C">C. Villagrasa-Canton</a>, <a href="/search/nucl-ex?searchtype=author&query=Boudard%2C+A">A. Boudard</a>, <a href="/search/nucl-ex?searchtype=author&query=Ducret%2C+J+-">J. -E. Ducret</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+B">B. Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Leray%2C+S">S. Leray</a>, <a href="/search/nucl-ex?searchtype=author&query=Volant%2C+C">C. Volant</a>, <a href="/search/nucl-ex?searchtype=author&query=Armbruster%2C+P">P. Armbruster</a>, <a href="/search/nucl-ex?searchtype=author&query=Enqvist%2C+T">T. Enqvist</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Helariutta%2C+K">K. Helariutta</a>, <a href="/search/nucl-ex?searchtype=author&query=Jurado%2C+B">B. Jurado</a>, <a href="/search/nucl-ex?searchtype=author&query=Ricciardi%2C+M+-">M. -V. Ricciardi</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K+-">K. -H. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Summerer%2C+K">K. Summerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Vives%2C+F">F. Vives</a>, <a href="/search/nucl-ex?searchtype=author&query=Yordanov%2C+O">O. Yordanov</a>, <a href="/search/nucl-ex?searchtype=author&query=Audouin%2C+L">L. Audouin</a>, <a href="/search/nucl-ex?searchtype=author&query=Bacri%2C+C+-">C. -O. Bacri</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferrant%2C+L">L. Ferrant</a>, <a href="/search/nucl-ex?searchtype=author&query=Napolitani%2C+P">P. Napolitani</a>, <a href="/search/nucl-ex?searchtype=author&query=Rejmund%2C+F">F. Rejmund</a>, <a href="/search/nucl-ex?searchtype=author&query=Stephan%2C+C">C. Stephan</a>, <a href="/search/nucl-ex?searchtype=author&query=Tassan-Got%2C+L">L. Tassan-Got</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">J. Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">E. Casarejos</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0612001v1-abstract-short" style="display: inline;"> The spallation residues produced in the bombardment of 56}Fe at 1.5, 1.0, 0.75, 0.5 and 0.3 A GeV on a liquid-hydrogen target have been measured using the reverse kinematics technique and the Fragment Separator at GSI (Darmstadt). This technique has permitted the full identification in charge and mass of all isotopes produced with cross-sections larger than 10^{-2} mb down to Z=8. Their individu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0612001v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0612001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0612001v1-abstract-full" style="display: none;"> The spallation residues produced in the bombardment of 56}Fe at 1.5, 1.0, 0.75, 0.5 and 0.3 A GeV on a liquid-hydrogen target have been measured using the reverse kinematics technique and the Fragment Separator at GSI (Darmstadt). This technique has permitted the full identification in charge and mass of all isotopes produced with cross-sections larger than 10^{-2} mb down to Z=8. Their individual production cross-sections and recoil velocities at the five energies are presented. Production cross-sections are compared to previously existing data and to empirical parametric formulas, often used in cosmic-ray astrophysics. The experimental data are also extensively compared to different combinations of intra-nuclear cascade and de-excitation models. It is shown that the yields of the lightest isotopes cannot be accounted for by standard evaporation models. The GEMINI model, which includes an asymmetric fission decay mode, gives an overall good agreement with the data. These experimental data can be directly used for the estimation of composition modifications and damages in materials containing iron in spallation sources. They are also useful for improving high precision cosmic-ray measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0612001v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0612001v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 December, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submited to Phys. Rev. C (10/2006)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C75:044603,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0610012">arXiv:nucl-ex/0610012</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0610012">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0610012">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0610012">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1742-6596/49/1/038">10.1088/1742-6596/49/1/038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the N=50 major shell effect close to $^{78}$Ni : First evidence of a weak coupling structure in $^{83}\_{32}$Ge$\_{51}$ and three-proton configuration states in $^{81}\_{31}$Ga$\_{50}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Verney%2C+D">D. Verney</a>, <a href="/search/nucl-ex?searchtype=author&query=Ibrahim%2C+F">F. Ibrahim</a>, <a href="/search/nucl-ex?searchtype=author&query=Perru%2C+O">O. Perru</a>, <a href="/search/nucl-ex?searchtype=author&query=Bajeat%2C+O">O. Bajeat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bourgeois%2C+C">C. Bourgeois</a>, <a href="/search/nucl-ex?searchtype=author&query=Ducourtieux%2C+M">M. Ducourtieux</a>, <a href="/search/nucl-ex?searchtype=author&query=Donzaud%2C+C">C. Donzaud</a>, <a href="/search/nucl-ex?searchtype=author&query=Essabaa%2C+S">S. Essabaa</a>, <a href="/search/nucl-ex?searchtype=author&query=Gales%2C+S">S. Gales</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaudefroy%2C+L">L. Gaudefroy</a>, <a href="/search/nucl-ex?searchtype=author&query=Guillemaud-Mueller%2C+D">D. Guillemaud-Mueller</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Lau%2C+C">C. Lau</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefort%2C+H">H. Lefort</a>, <a href="/search/nucl-ex?searchtype=author&query=Blanc%2C+F+L">F. Le Blanc</a>, <a href="/search/nucl-ex?searchtype=author&query=Mueller%2C+A+C">A. C. Mueller</a>, <a href="/search/nucl-ex?searchtype=author&query=Pougheon%2C+F">F. Pougheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Roussiere%2C+B">B. Roussiere</a>, <a href="/search/nucl-ex?searchtype=author&query=Sauvage%2C+J">J. Sauvage</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0610012v1-abstract-short" style="display: inline;"> New levels were attributed to $^{81}\_{31}$Ga$\_{50}$ and $^{83}\_{32}$Ge$\_{51}$ which were fed by the $尾$-decay of their respective mother nuclei $^{81}\_{30}$Zn$\_{51}$ and $^{83}\_{31}$Ga$\_{52}$ produced by fission at the "PARRNe" ISOL set-up installed at the Tandem accelerator of the Institut de Physique Nucl茅aire, Orsay. We show that the low energy structure of $^{81}\_{31}$Ga$\_{50}$ and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0610012v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0610012v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0610012v1-abstract-full" style="display: none;"> New levels were attributed to $^{81}\_{31}$Ga$\_{50}$ and $^{83}\_{32}$Ge$\_{51}$ which were fed by the $尾$-decay of their respective mother nuclei $^{81}\_{30}$Zn$\_{51}$ and $^{83}\_{31}$Ga$\_{52}$ produced by fission at the "PARRNe" ISOL set-up installed at the Tandem accelerator of the Institut de Physique Nucl茅aire, Orsay. We show that the low energy structure of $^{81}\_{31}$Ga$\_{50}$ and $^{83}\_{32}$Ge$\_{51}$ can easily be explained within the natural hypothesis of a strong energy gap at N=50 and a doubly-magic character for $^{78}$Ni. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0610012v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0610012v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">2 pages, pdf file, To be published in the Proceedings of "International Symposium on Structure of Exotic Nuclei and Nuclear Forces (SENUF 06)", March 2006, Tokyo, Japan</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J.Phys.Conf.Ser.49:170-171,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0508014">arXiv:nucl-ex/0508014</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0508014">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0508014">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0508014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.73.015806">10.1103/PhysRevC.73.015806 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Low-energy cross section of the 7Be(p,g)8B solar fusion reaction from Coulomb dissociation of 8B </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Schuemann%2C+F">F. Schuemann</a>, <a href="/search/nucl-ex?searchtype=author&query=Typel%2C+S">S. Typel</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Uhlig%2C+F">F. Uhlig</a>, <a href="/search/nucl-ex?searchtype=author&query=Suemmerer%2C+K">K. Suemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boettcher%2C+I">I. Boettcher</a>, <a href="/search/nucl-ex?searchtype=author&query=Cortina%2C+D">D. Cortina</a>, <a href="/search/nucl-ex?searchtype=author&query=Foerster%2C+A">A. Foerster</a>, <a href="/search/nucl-ex?searchtype=author&query=Gai%2C+M">M. Gai</a>, <a href="/search/nucl-ex?searchtype=author&query=Geissel%2C+H">H. Geissel</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U. Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Grosse%2C+E">E. Grosse</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Koczon%2C+P">P. Koczon</a>, <a href="/search/nucl-ex?searchtype=author&query=Kohlmeyer%2C+B">B. Kohlmeyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Kulessa%2C+R">R. Kulessa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kumagai%2C+H">H. Kumagai</a>, <a href="/search/nucl-ex?searchtype=author&query=Kurz%2C+N">N. Kurz</a>, <a href="/search/nucl-ex?searchtype=author&query=Menzel%2C+M">M. Menzel</a>, <a href="/search/nucl-ex?searchtype=author&query=Motobayashi%2C+T">T. Motobayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Oeschler%2C+H">H. Oeschler</a>, <a href="/search/nucl-ex?searchtype=author&query=Ozawa%2C+A">A. Ozawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Ploskon%2C+M">M. Ploskon</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokopowicz%2C+W">W. Prokopowicz</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwab%2C+E">E. Schwab</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0508014v2-abstract-short" style="display: inline;"> Final results from an exclusive measurement of the Coulomb breakup of 8B into 7Be+p at 254 A MeV are reported. Energy-differential Coulomb-breakup cross sections are analyzed using a potential model of 8B and first-order perturbation theory. The deduced astrophysical S_17 factors are in good agreement with the most recent direct 7Be(p,gamma)8B measurements and follow closely the energy dependenc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0508014v2-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0508014v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0508014v2-abstract-full" style="display: none;"> Final results from an exclusive measurement of the Coulomb breakup of 8B into 7Be+p at 254 A MeV are reported. Energy-differential Coulomb-breakup cross sections are analyzed using a potential model of 8B and first-order perturbation theory. The deduced astrophysical S_17 factors are in good agreement with the most recent direct 7Be(p,gamma)8B measurements and follow closely the energy dependence predicted by the cluster-model description of 8B by Descouvemont. We extract a zero-energy S_17 factor of 20.6 +- 0.8 (stat) +- 1.2 (syst) eV b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0508014v2-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0508014v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 November, 2005; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 August, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages including 16 figures, LaTeX, accepted for publication in Physical Review C. Minor changes in text and layout</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C73:015806,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0308024">arXiv:nucl-ex/0308024</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0308024">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0308024">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0308024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.68.025804">10.1103/PhysRevC.68.025804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cross sections relevant to gamma-ray line emission in solar flares: $^3$He-induced reactions on $^{16}$O nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Duprat%2C+J">J. Duprat</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Assuncao%2C+M">M. Assuncao</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Engrand%2C+C">C. Engrand</a>, <a href="/search/nucl-ex?searchtype=author&query=Gounelle%2C+M">M. Gounelle</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre%2C+A">A. Lefebvre</a>, <a href="/search/nucl-ex?searchtype=author&query=Porquet%2C+M+-">M. -G. Porquet</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Sereville%2C+N">N. De Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Thibaud%2C+J+-">J. -P. Thibaud</a>, <a href="/search/nucl-ex?searchtype=author&query=Bourgeois%2C+C">C. Bourgeois</a>, <a href="/search/nucl-ex?searchtype=author&query=Chabot%2C+M">M. Chabot</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Scarpaci%2C+J+-">J. -A. Scarpaci</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0308024v1-abstract-short" style="display: inline;"> Gamma-ray production cross sections have been measured for gamma-ray lines copiously emitted in the $^3$He bombardment of $^{16}$O nuclei: the 937, 1042 and 1081 keV lines of $^{18}$F and the 1887 keV line of $^{18}$Ne. Four Ge detectors with BGO shielding for Compton suppression were used to measure the angular distributions of the gamma-rays. The excitation functions have been obtained for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308024v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0308024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0308024v1-abstract-full" style="display: none;"> Gamma-ray production cross sections have been measured for gamma-ray lines copiously emitted in the $^3$He bombardment of $^{16}$O nuclei: the 937, 1042 and 1081 keV lines of $^{18}$F and the 1887 keV line of $^{18}$Ne. Four Ge detectors with BGO shielding for Compton suppression were used to measure the angular distributions of the gamma-rays. The excitation functions have been obtained for $^3$He bombarding energies from 3.7 to 36 MeV. Total cross sections are tabulated for calculations relevant to gamma-ray astronomy. The importance of these lines as diagnosis for the presence and properties of accelerated $^3$He in solar flares is discussed in light of the measured cross sections. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308024v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0308024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 August, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Phys. Rev. C68 (2003) 0258XX, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev. C68 (2003) 025804 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0304014">arXiv:nucl-ex/0304014</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0304014">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0304014">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0304014">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.67.052801">10.1103/PhysRevC.67.052801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> D(18F,pa)15N reaction applied to nova gamma-ray emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=de+Sereville%2C+N">N. de Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Angulo%2C+C">C. Angulo</a>, <a href="/search/nucl-ex?searchtype=author&query=Assuncao%2C+M">M. Assuncao</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Bouzid%2C+B">B. Bouzid</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Couder%2C+M">M. Couder</a>, <a href="/search/nucl-ex?searchtype=author&query=Demaret%2C+P">P. Demaret</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Figuera%2C+P">P. Figuera</a>, <a href="/search/nucl-ex?searchtype=author&query=Fortier%2C+S">S. Fortier</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaelens%2C+M">M. Gaelens</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Labar%2C+D">D. Labar</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre%2C+A">A. Lefebvre</a>, <a href="/search/nucl-ex?searchtype=author&query=Leleux%2C+P">P. Leleux</a>, <a href="/search/nucl-ex?searchtype=author&query=Loiselet%2C+M">M. Loiselet</a>, <a href="/search/nucl-ex?searchtype=author&query=Ninane%2C+A">A. Ninane</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Ryckewaert%2C+G">G. Ryckewaert</a>, <a href="/search/nucl-ex?searchtype=author&query=Smirnova%2C+N">N. Smirnova</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Thibaud%2C+J+-">J. -P. Thibaud</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0304014v1-abstract-short" style="display: inline;"> The 18F(p,alpha)15O reaction is recognized to be one of the most important reactions for nova gamma-ray astronomy as it governs the early E <= 511keV gamma emission. However in the nova temperature regime, its rate remains largely uncertain due to unknown low-energy resonance strengths. We report here the measurement of the D(18F,p)19F(alpha)15N one-nucleon transfer reaction, induced by a 14 MeV… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0304014v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0304014v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0304014v1-abstract-full" style="display: none;"> The 18F(p,alpha)15O reaction is recognized to be one of the most important reactions for nova gamma-ray astronomy as it governs the early E <= 511keV gamma emission. However in the nova temperature regime, its rate remains largely uncertain due to unknown low-energy resonance strengths. We report here the measurement of the D(18F,p)19F(alpha)15N one-nucleon transfer reaction, induced by a 14 MeV 18F radioactive beam impinging on a CD2 target; outgoing protons and 15N (or alpha-particles) were detected in coincidence in two silicon strip detectors. A DWBA analysis of the data resulted in new limits to the contribution of low-energy resonances to the rate of the 18F(p,alpha)15O reaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0304014v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0304014v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Rapid Communication to appear in Phys. Rev. C., 4 pages and 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C67:052801,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0304011">arXiv:nucl-ex/0304011</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0304011">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0304011">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0304011">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.90.232501">10.1103/PhysRevLett.90.232501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Coulomb dissociation of 8B and the low-energy cross section of the 7Be(p,gamma)8B solar fusion reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Schuemann%2C+F">F. Schuemann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Typel%2C+S">S. Typel</a>, <a href="/search/nucl-ex?searchtype=author&query=Uhlig%2C+F">F. Uhlig</a>, <a href="/search/nucl-ex?searchtype=author&query=Suemmerer%2C+K">K. Suemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boettcher%2C+I">I. Boettcher</a>, <a href="/search/nucl-ex?searchtype=author&query=Cortina%2C+D">D. Cortina</a>, <a href="/search/nucl-ex?searchtype=author&query=Foerster%2C+A">A. Foerster</a>, <a href="/search/nucl-ex?searchtype=author&query=Gai%2C+M">M. Gai</a>, <a href="/search/nucl-ex?searchtype=author&query=Geissel%2C+H">H. Geissel</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U. Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Koczon%2C+P">P. Koczon</a>, <a href="/search/nucl-ex?searchtype=author&query=Kohlmeyer%2C+B">B. Kohlmeyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Kulessa%2C+R">R. Kulessa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kumagai%2C+H">H. Kumagai</a>, <a href="/search/nucl-ex?searchtype=author&query=Kurz%2C+N">N. Kurz</a>, <a href="/search/nucl-ex?searchtype=author&query=Menzel%2C+M">M. Menzel</a>, <a href="/search/nucl-ex?searchtype=author&query=Motobayashi%2C+T">T. Motobayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Oeschler%2C+H">H. Oeschler</a>, <a href="/search/nucl-ex?searchtype=author&query=Ozawa%2C+A">A. Ozawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Ploskon%2C+M">M. Ploskon</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokopowicz%2C+W">W. Prokopowicz</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwab%2C+E">E. Schwab</a>, <a href="/search/nucl-ex?searchtype=author&query=Senger%2C+P">P. Senger</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0304011v2-abstract-short" style="display: inline;"> An exclusive measurement of the Coulomb breakup of 8B into 7Be+p at 254 A MeV allowed to study the angular correlations of the breakup particles. These correlations demonstrate clearly that E1 multipolarity dominates and that E2 multipolarity can be neglected. By using a simple single-particle model for 8B and treating the breakup in first-order perturbation theory, we extract a zero-energy S fa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0304011v2-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0304011v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0304011v2-abstract-full" style="display: none;"> An exclusive measurement of the Coulomb breakup of 8B into 7Be+p at 254 A MeV allowed to study the angular correlations of the breakup particles. These correlations demonstrate clearly that E1 multipolarity dominates and that E2 multipolarity can be neglected. By using a simple single-particle model for 8B and treating the breakup in first-order perturbation theory, we extract a zero-energy S factor of S-(17)(0) = 18.6 +- 1.2 +- 1.0 eV b. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0304011v2-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0304011v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 June, 2003; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 April, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages including 4 figures, LaTeX</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.90:232501,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0209017">arXiv:nucl-ex/0209017</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0209017">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0209017">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0209017">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/S0375-9474(03)00725-5">10.1016/S0375-9474(03)00725-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the ^18F(p, alpha)^15O reaction for application to nova gamma-ray emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=de+Sereville%2C+N">N. de Sereville</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Angulo%2C+C">C. Angulo</a>, <a href="/search/nucl-ex?searchtype=author&query=Assuncao%2C+M">M. Assuncao</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Bouzid%2C+B">B. Bouzid</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Couder%2C+M">M. Couder</a>, <a href="/search/nucl-ex?searchtype=author&query=Demaret%2C+P">P. Demaret</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Figuera%2C+P">P. Figuera</a>, <a href="/search/nucl-ex?searchtype=author&query=Fortier%2C+S">S. Fortier</a>, <a href="/search/nucl-ex?searchtype=author&query=Gaelens%2C+M">M. Gaelens</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Labar%2C+D">D. Labar</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre%2C+A">A. Lefebvre</a>, <a href="/search/nucl-ex?searchtype=author&query=Leleux%2C+P">P. Leleux</a>, <a href="/search/nucl-ex?searchtype=author&query=Loiselet%2C+M">M. Loiselet</a>, <a href="/search/nucl-ex?searchtype=author&query=Ninane%2C+A">A. Ninane</a>, <a href="/search/nucl-ex?searchtype=author&query=Ouichaoui%2C+S">S. Ouichaoui</a>, <a href="/search/nucl-ex?searchtype=author&query=Ryckewaert%2C+G">G. Ryckewaert</a>, <a href="/search/nucl-ex?searchtype=author&query=Smirnova%2C+N">N. Smirnova</a>, <a href="/search/nucl-ex?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/nucl-ex?searchtype=author&query=Thibaud%2C+J+-">J. -P. Thibaud</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0209017v1-abstract-short" style="display: inline;"> The ^18F(p, alpha)^15O reaction is recognized as one of the most important reaction for nova gamma-ray astronomy as it governs the early =< 511 keV emission. However, its rate remains largely uncertain at nova temperatures due to unknown low-energy resonance strengths. In order to better constrain this reaction rate, we have studied the one-nucleon transfer reaction, D(^18F,p alpha)^15N, at the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0209017v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0209017v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0209017v1-abstract-full" style="display: none;"> The ^18F(p, alpha)^15O reaction is recognized as one of the most important reaction for nova gamma-ray astronomy as it governs the early =< 511 keV emission. However, its rate remains largely uncertain at nova temperatures due to unknown low-energy resonance strengths. In order to better constrain this reaction rate, we have studied the one-nucleon transfer reaction, D(^18F,p alpha)^15N, at the CRC-RIB facility at Louvain La Neuve. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0209017v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0209017v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to The Seventh International Symposium on Nuclei in the Cosmos</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys. 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