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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=Bemmerer%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Bemmerer%2C+D&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Bemmerer%2C+D&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/2411.05053">arXiv:2411.05053</a> <span> [<a href="https://arxiv.org/pdf/2411.05053">pdf</a>, <a href="https://arxiv.org/format/2411.05053">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.2021.165081">10.1016/j.nima.2021.165081 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the LUNA neutron detector array for the measurement of the 13C(a,n)16O reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</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="2411.05053v1-abstract-short" style="display: inline;"> We introduce the LUNA neutron detector array developed for the investigation of the 13C(a,n)16O reaction towards its astrophysical s-process Gamow peak in the low-background environment of the Laboratori Nazionali del Gran Sasso (LNGS). Eighteen 3He counters are arranged in two different configurations (in a vertical and a horizontal orientation) to optimize neutron detection effciency, target han… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05053v1-abstract-full').style.display = 'inline'; document.getElementById('2411.05053v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.05053v1-abstract-full" style="display: none;"> We introduce the LUNA neutron detector array developed for the investigation of the 13C(a,n)16O reaction towards its astrophysical s-process Gamow peak in the low-background environment of the Laboratori Nazionali del Gran Sasso (LNGS). Eighteen 3He counters are arranged in two different configurations (in a vertical and a horizontal orientation) to optimize neutron detection effciency, target handling and target cooling over the investigated energy range Ea;lab = 300 - 400 keV (En = 2.2 - 2.6 MeV in emitted neutron energy). As a result of the deep underground location, the passive shielding of the setup and active background suppression using pulse shape discrimination, we reached a total background rate of 1.23 +- 0.12 counts/hour. This resulted in an improvement of two orders of magnitude over the state of the art allowing a direct measurement of the 13C(a,n)16O cross-section down to Ea;lab = 300 keV. The absolute neutron detection efficiency of the setup was determined using the 51V(p,n)51Cr reaction and an AmBe radioactive source, and completed with a Geant4 simulation. We determined a (34+-3) % and (38+-3) % detection efficiency for the vertical and horizontal configurations, respectively, for En = 2.4 MeV neutrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.05053v1-abstract-full').style.display = 'none'; document.getElementById('2411.05053v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures, to be published in NIMA</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 994 (2021) 165081 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03015">arXiv:2408.03015</a> <span> [<a href="https://arxiv.org/pdf/2408.03015">pdf</a>, <a href="https://arxiv.org/format/2408.03015">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.133.052701">10.1103/PhysRevLett.133.052701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First direct measurement of the 64.5 keV resonance strength in $^{17}$O(p,$纬$)$^{18}$F reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Gesu%C3%A8%2C+R+M">R. M. Gesu猫</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapagnani%2C+D">D. Rapagnani</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Ananna%2C+C">C. Ananna</a>, <a href="/search/nucl-ex?searchtype=author&query=Barbieri%2C+L">L. Barbieri</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Campostrini%2C+M">M. Campostrini</a>, <a href="/search/nucl-ex?searchtype=author&query=Casaburo%2C+F">F. Casaburo</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Compagnucci%2C+A">A. Compagnucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Gregorio%2C+G+M">G. M. De Gregorio</a>, <a href="/search/nucl-ex?searchtype=author&query=Dell%27Aquila%2C+D">D. Dell'Aquila</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a> , et al. (28 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="2408.03015v1-abstract-short" style="display: inline;"> The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK $<$ T $<$ 80 MK) the $^{17}$O(p,$纬$)$^{18}$F reaction rate is dominated by the poorly constrained 64.5~keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensiti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03015v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03015v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03015v1-abstract-full" style="display: none;"> The CNO cycle is one of the most important nuclear energy sources in stars. At temperatures of hydrostatic H-burning (20 MK $<$ T $<$ 80 MK) the $^{17}$O(p,$纬$)$^{18}$F reaction rate is dominated by the poorly constrained 64.5~keV resonance. Here we report on the first direct measurements of its resonance strength and of the direct capture contribution at 142 keV, performed with a new high sensitivity setup at LUNA. The present resonance strength of $蠅纬_{(p, 纬)}$\textsuperscript{bare} = (30 $\pm$ 6\textsubscript{stat} $\pm$ 2\textsubscript{syst})~peV is about a factor of 2 higher than the values in literature, leading to a $螕$\textsubscript{p}\textsuperscript{bare} = (34 $\pm$ 7\textsubscript{stat} $\pm$ 3\textsubscript{syst})~neV, in agreement with LUNA result from the (p,$伪$) channel. Such agreement strengthen our understanding of the oxygen isotopic ratios measured in red giant stars and in O-rich presolar grains. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03015v1-abstract-full').style.display = 'none'; document.getElementById('2408.03015v1-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.06470">arXiv:2405.06470</a> <span> [<a href="https://arxiv.org/pdf/2405.06470">pdf</a>, <a href="https://arxiv.org/format/2405.06470">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey 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"> Solar fusion III: New data and theory for hydrogen-burning stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acharya%2C+B">B. Acharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Balantekin%2C+A+B">A. B. Balantekin</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C+A">C. A. Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Brune%2C+C+R">C. R. Brune</a>, <a href="/search/nucl-ex?searchtype=author&query=Buompane%2C+R">R. Buompane</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+J+W">J. W. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Colgan%2C+J">J. Colgan</a>, <a href="/search/nucl-ex?searchtype=author&query=Czarnecki%2C+A">A. Czarnecki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davids%2C+B">B. Davids</a>, <a href="/search/nucl-ex?searchtype=author&query=deBoer%2C+R+J">R. J. deBoer</a>, <a href="/search/nucl-ex?searchtype=author&query=Delahaye%2C+F">F. Delahaye</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+A">A. Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Johnson%2C+M+G">M. Gatu Johnson</a>, <a href="/search/nucl-ex?searchtype=author&query=Gazit%2C+D">D. Gazit</a>, <a href="/search/nucl-ex?searchtype=author&query=Gialanella%2C+L">L. Gialanella</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U. Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Guffanti%2C+D">D. Guffanti</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Hambleton%2C+K">K. Hambleton</a>, <a href="/search/nucl-ex?searchtype=author&query=Haxton%2C+W+C">W. C. Haxton</a> , et al. (25 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="2405.06470v1-abstract-short" style="display: inline;"> In stars that lie on the main sequence in the Hertzsprung Russel diagram, like our sun, hydrogen is fused to helium in a number of nuclear reaction chains and series, such as the proton-proton chain and the carbon-nitrogen-oxygen cycles. Precisely determined thermonuclear rates of these reactions lie at the foundation of the standard solar model. This review, the third decadal evaluation of the nu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06470v1-abstract-full').style.display = 'inline'; document.getElementById('2405.06470v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.06470v1-abstract-full" style="display: none;"> In stars that lie on the main sequence in the Hertzsprung Russel diagram, like our sun, hydrogen is fused to helium in a number of nuclear reaction chains and series, such as the proton-proton chain and the carbon-nitrogen-oxygen cycles. Precisely determined thermonuclear rates of these reactions lie at the foundation of the standard solar model. This review, the third decadal evaluation of the nuclear physics of hydrogen-burning stars, is motivated by the great advances made in recent years by solar neutrino observatories, putting experimental knowledge of the proton-proton chain neutrino fluxes in the few-percent precision range. The basis of the review is a one-week community meeting held in July 2022 in Berkeley, California, and many subsequent digital meetings and exchanges. Each of the relevant reactions of solar and quiescent stellar hydrogen burning is reviewed here, from both theoretical and experimental perspectives. Recommendations for the state of the art of the astrophysical S-factor and its uncertainty are formulated for each of them. Several other topics of paramount importance for the solar model are reviewed, as well: recent and future neutrino experiments, electron screening, radiative opacities, and current and upcoming experimental facilities. In addition to reaction-specific recommendations, also general recommendations are formed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06470v1-abstract-full').style.display = 'none'; document.getElementById('2405.06470v1-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 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">85 pages, 15 figures. To be submitted to Reviews of Modern Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> N3AS-24-016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04089">arXiv:2311.04089</a> <span> [<a href="https://arxiv.org/pdf/2311.04089">pdf</a>, <a href="https://arxiv.org/format/2311.04089">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"> First measurement of the low-energy direct capture in 20Ne(p, 纬)21Na and improved energy and strength of the Ecm = 368 keV resonance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Masha%2C+E">E. Masha</a>, <a href="/search/nucl-ex?searchtype=author&query=Barbieri%2C+L">L. Barbieri</a>, <a href="/search/nucl-ex?searchtype=author&query=Skowronski%2C+J">J. Skowronski</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Ananna%2C+C">C. Ananna</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Campostrini%2C+M">M. Campostrini</a>, <a href="/search/nucl-ex?searchtype=author&query=Casaburo%2C+F">F. Casaburo</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciapponi%2C+A">A. Ciapponi</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Compagnucci%2C+A">A. Compagnucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a> , et al. (26 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="2311.04089v1-abstract-short" style="display: inline;"> The $\mathrm{^{20}Ne(p, 纬)^{21}Na}$ reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below $E\rm_{cm} = 352$~keV, and of the contribution from the $E^{\rm }_{cm} = 368$~keV resonance, which dominates the reaction rate at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04089v1-abstract-full').style.display = 'inline'; document.getElementById('2311.04089v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04089v1-abstract-full" style="display: none;"> The $\mathrm{^{20}Ne(p, 纬)^{21}Na}$ reaction is the slowest in the NeNa cycle and directly affects the abundances of the Ne and Na isotopes in a variety of astrophysical sites. Here we report the measurement of its direct capture contribution, for the first time below $E\rm_{cm} = 352$~keV, and of the contribution from the $E^{\rm }_{cm} = 368$~keV resonance, which dominates the reaction rate at $T=0.03-1.00$~GK. The experiment was performed deep underground at the Laboratory for Underground Nuclear Astrophysics, using a high-intensity proton beam and a windowless neon gas target. Prompt $纬$ rays from the reaction were detected with two high-purity germanium detectors. We obtain a resonance strength $蠅纬~=~(0.112 \pm 0.002_{\rm stat}~\pm~0.005_{\rm sys})$~meV, with an uncertainty a factor of $3$ smaller than previous values. Our revised reaction rate is 20\% lower than previously adopted at $T < 0.1$~GK and agrees with previous estimates at temperatures $T \geq 0.1$~GK. Initial astrophysical implications are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04089v1-abstract-full').style.display = 'none'; document.getElementById('2311.04089v1-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 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">8 pages, 4 figures, accepted to PRC (letter)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.16098">arXiv:2308.16098</a> <span> [<a href="https://arxiv.org/pdf/2308.16098">pdf</a>, <a href="https://arxiv.org/format/2308.16098">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.131.162701">10.1103/PhysRevLett.131.162701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New proton-capture rates on carbon isotopes and their impact on the astrophysical $^{12}\mathrm{C}/{}^{13}\mathrm{C}$ ratio </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Skowronski%2C+J">J. Skowronski</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Ananna%2C+C">C. Ananna</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Campostrini%2C+M">M. Campostrini</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Compagnucci%2C+A">A. Compagnucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a> , et al. (21 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="2308.16098v1-abstract-short" style="display: inline;"> The ${}^{12}\mathrm{C}/{}^{13}\mathrm{C}$ ratio is a significant indicator of nucleosynthesis and mixing processes during hydrogen burning in stars. Its value mainly depends on the relative rates of the ${}^{12}\mathrm{C}(p,纬){}^{13}\mathrm{N}$ and ${}^{13}\mathrm{C}(p,纬){}^{14}\mathrm{N}$ reactions. Both reactions have been studied at the Laboratory for Underground Nuclear Astrophysics (LUNA) in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16098v1-abstract-full').style.display = 'inline'; document.getElementById('2308.16098v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.16098v1-abstract-full" style="display: none;"> The ${}^{12}\mathrm{C}/{}^{13}\mathrm{C}$ ratio is a significant indicator of nucleosynthesis and mixing processes during hydrogen burning in stars. Its value mainly depends on the relative rates of the ${}^{12}\mathrm{C}(p,纬){}^{13}\mathrm{N}$ and ${}^{13}\mathrm{C}(p,纬){}^{14}\mathrm{N}$ reactions. Both reactions have been studied at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy down to the lowest energies to date ($E_\mathrm{c.m.} = 60\,\mathrm{keV}$) reaching for the first time the high energy tail of hydrogen burning in the shell of giant stars. Our cross sections, obtained with both prompt $纬$-ray detection and activation measurements, are the most precise to date with overall systematic uncertainties of $7-8\%$. Compared with most of the literature, our results are systematically lower, by $25\%$ for the ${}^{12}\mathrm{C}(p,纬){}^{13}\mathrm{N}$ reaction and by $30\%$ for ${}^{13}\mathrm{C}(p,纬){}^{14}\mathrm{N}$. We provide the most precise value up to now of $(3.6 \pm 0.4)$ in the $20-140\,\mathrm{MK}$ range for the lowest possible ${}^{12}\mathrm{C}/{}^{13}\mathrm{C}$ ratio that can be produced during H burning in giant stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.16098v1-abstract-full').style.display = 'none'; document.getElementById('2308.16098v1-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> 30 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Submitted to Phys. Rev. Lett</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, 162701 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.09022">arXiv:2306.09022</a> <span> [<a href="https://arxiv.org/pdf/2306.09022">pdf</a>, <a href="https://arxiv.org/format/2306.09022">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.107.L062801">10.1103/PhysRevC.107.L062801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved $S$-factor of the $^{12}$C(p,$纬$)$^{13}$N reaction at $E\,=\,$320-620~keV and the 422~keV resonance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Skowronski%2C+J">J. Skowronski</a>, <a href="/search/nucl-ex?searchtype=author&query=Masha%2C+E">E. Masha</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Babu%2C+H">H. Babu</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Z. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapagnani%2C+D">D. Rapagnani</a>, <a href="/search/nucl-ex?searchtype=author&query=R%C3%BCmmler%2C+S">S. R眉mmler</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Sidhu%2C+R+S">R. S. Sidhu</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Turkat%2C+S">S. Turkat</a>, <a href="/search/nucl-ex?searchtype=author&query=Yadav%2C+A">A. Yadav</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="2306.09022v1-abstract-short" style="display: inline;"> The 12C(p,纬)13N reaction is the onset process of both the CNO and Hot CNO cycles that drive massive star, Red and Asymptotic Giant Branch star and novae nucleosynthesis. The 12C(p,纬)13N rate affects the final abundances of the stable 12,13C nuclides, with ramifications for meteoritic carbon isotopic abundances and the s-process neutron source strength. Here, a new underground measurement of the 12… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09022v1-abstract-full').style.display = 'inline'; document.getElementById('2306.09022v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.09022v1-abstract-full" style="display: none;"> The 12C(p,纬)13N reaction is the onset process of both the CNO and Hot CNO cycles that drive massive star, Red and Asymptotic Giant Branch star and novae nucleosynthesis. The 12C(p,纬)13N rate affects the final abundances of the stable 12,13C nuclides, with ramifications for meteoritic carbon isotopic abundances and the s-process neutron source strength. Here, a new underground measurement of the 12C(p,纬)13N cross-section is reported. The present data, obtained at the Felsenkeller shallow-underground laboratory in Dresden (Germany), encompass the 320-620 keV center of mass energy range to include the wide and poorly constrained E = 422 keV resonance that dominates the rate at high temperatures. This work S-factor results, lower than literature by 25%, are included in a new comprehensive R-matrix fit, and the energy of the 1+ first excited state of 13N is found to be 2369.6(4) keV, with radiative and proton width of 0.49(3) eV and 34.9(2) keV respectively. A new reaction rate, based on present R-matrix fit and extrapolation, is suggested. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09022v1-abstract-full').style.display = 'none'; document.getElementById('2306.09022v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Submitted to Phys. Rev. C (Letter)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 107, L062801 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.09421">arXiv:2212.09421</a> <span> [<a href="https://arxiv.org/pdf/2212.09421">pdf</a>, <a href="https://arxiv.org/format/2212.09421">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.2022.167972">10.1016/j.nima.2022.167972 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of a possible silicon photomultiplier based readout of the large plastic scintillator neutron detector NeuLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">Thomas Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Weinberger%2C+D">David Weinberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">Konstanze Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Ga%C5%A1pari%C4%87%2C+I">Igor Ga拧pari膰</a>, <a href="/search/nucl-ex?searchtype=author&query=Stach%2C+D">Daniel Stach</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">Andreas Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="2212.09421v1-abstract-short" style="display: inline;"> The NeuLAND (New Large-Area Neutron Detector) plastic-scintillator-based time-of-flight detector for 0.1-1.6 GeV neutrons is currently under construction at the Facility for Antiproton and Ion Research (FAIR), Darmstadt, Germany. In its final configuration, NeuLAND will consist of 3000 2.7 m $\times$ 5 cm $\times$ 5 cm big plastic scintillator bars that are read out on each end by fast timing phot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09421v1-abstract-full').style.display = 'inline'; document.getElementById('2212.09421v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.09421v1-abstract-full" style="display: none;"> The NeuLAND (New Large-Area Neutron Detector) plastic-scintillator-based time-of-flight detector for 0.1-1.6 GeV neutrons is currently under construction at the Facility for Antiproton and Ion Research (FAIR), Darmstadt, Germany. In its final configuration, NeuLAND will consist of 3000 2.7 m $\times$ 5 cm $\times$ 5 cm big plastic scintillator bars that are read out on each end by fast timing photomultipliers. Here, data from a comprehensive study of an alternative light readout scheme using silicon photomultipliers (SiPM) are reported. For this purpose, a NeuLAND bar was instrumented on each end with a SiPM-based prototype of the same geometry as a 1'' photomultiplier tube, including four 6 $\times$ 6 mm$^2$ SiPMs, amplifiers, high voltage supply, and microcontroller. Tests were carried out using the 35 MeV electron beam from the superconducting Electron Linac for beams with high Brilliance and low Emittance (ELBE) with its picosecond-level time jitter in two different modes of operation, namely parasitic mode with one electron per bunch and single-user mode with 1-60 electrons per bunch. Acqiris fast digitisers were used for data acquisition. In addition, off-beam tests using cosmic rays and the NeuLAND data acquisition scheme have been carried out. Typical time resolutions of $蟽_t\leq$ 120 ps were found for $\geq$95% efficiency for minimum ionising particles, improving on previous work at ELBE and exceeding the NeuLAND timing goal of $蟽_t$ < 150 ps. Over a range of 10-300 MeV deposited energy in the NeuLAND bar, the gain was found to deviate by $\leq$10% ($\leq$20%) from linearity for 35 mm (75 mm) SiPM pitch, respectively, satisfactory for calorimetric use of the full NeuLAND detector. The dark rate of the prototype studied was found to be lower than the expected cosmic-ray induced background in NeuLAND. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.09421v1-abstract-full').style.display = 'none'; document.getElementById('2212.09421v1-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 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">Submitted to Nucl. Inst. Meth. A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Inst. Meth. A 1048, 167972 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.06302">arXiv:2212.06302</a> <span> [<a href="https://arxiv.org/pdf/2212.06302">pdf</a>, <a href="https://arxiv.org/format/2212.06302">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> <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/10.1038/s41467-023-40121-3">10.1038/s41467-023-40121-3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for $^{22}$Na in novae supported by a novel method for measuring femtosecond nuclear lifetimes </p> <p class="authors"> <span class="search-hit">Authors:</span> <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=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Jos%C3%A9%2C+J">J. Jos茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Michelagnoli%2C+C">C. Michelagnoli</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=Kim%2C+Y+H">Y. H. Kim</a>, <a href="/search/nucl-ex?searchtype=author&query=Lemasson%2C+A">A. Lemasson</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimaraes%2C+V">V. Guimaraes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrientos%2C+D">D. Barrientos</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</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=Bottger%2C+R">R. Bottger</a>, <a href="/search/nucl-ex?searchtype=author&query=Boulay%2C+F">F. Boulay</a>, <a href="/search/nucl-ex?searchtype=author&query=Bracco%2C+A">A. Bracco</a>, <a href="/search/nucl-ex?searchtype=author&query=Celikovic%2C+I">I. Celikovic</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=Delafosse%2C+C">C. Delafosse</a>, <a href="/search/nucl-ex?searchtype=author&query=Domingo-Pardo%2C+C">C. Domingo-Pardo</a>, <a href="/search/nucl-ex?searchtype=author&query=Dudouet%2C+J">J. Dudouet</a>, <a href="/search/nucl-ex?searchtype=author&query=Eberth%2C+J">J. Eberth</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulop%2C+Z">Z. Fulop</a>, <a href="/search/nucl-ex?searchtype=author&query=Gonzalez%2C+V">V. Gonzalez</a>, <a href="/search/nucl-ex?searchtype=author&query=Goupil%2C+J">J. Goupil</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="2212.06302v1-abstract-short" style="display: inline;"> Classical novae are thermonuclear explosions in stellar binary systems, and important sources of $^{26}$Al and $^{22}$Na. While gamma rays from the decay of the former radioisotope have been observed throughout the Galaxy, $^{22}$Na remains untraceable. The half-life of $^{22}$Na (2.6 yr) would allow the observation of its 1.275 MeV gamma-ray line from a cosmic source. However, the prediction of s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06302v1-abstract-full').style.display = 'inline'; document.getElementById('2212.06302v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.06302v1-abstract-full" style="display: none;"> Classical novae are thermonuclear explosions in stellar binary systems, and important sources of $^{26}$Al and $^{22}$Na. While gamma rays from the decay of the former radioisotope have been observed throughout the Galaxy, $^{22}$Na remains untraceable. The half-life of $^{22}$Na (2.6 yr) would allow the observation of its 1.275 MeV gamma-ray line from a cosmic source. However, the prediction of such an observation requires good knowledge of the nuclear reactions involved in the production and destruction of this nucleus. The $^{22}$Na($p,纬$)$^{23}$Mg reaction remains the only source of large uncertainty about the amount of $^{22}$Na ejected. Its rate is dominated by a single resonance on the short-lived state at 7785.0(7) keV in $^{23}$Mg. In the present work, a combined analysis of particle-particle correlations and velocity-difference profiles is proposed to measure femtosecond nuclear lifetimes. The application of this novel method to the study of the $^{23}$Mg states, combining magnetic and highly-segmented tracking gamma-ray spectrometers, places strong limits on the amount of $^{22}$Na produced in novae, explains its non-observation to date in gamma rays (flux < 2.5x$10^{-4}$ ph/(cm$^2$s)), and constrains its detectability with future space-borne observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.06302v1-abstract-full').style.display = 'none'; document.getElementById('2212.06302v1-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 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">18 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> Nature Communications 14, 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.15218">arXiv:2210.15218</a> <span> [<a href="https://arxiv.org/pdf/2210.15218">pdf</a>, <a href="https://arxiv.org/format/2210.15218">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/10.1051/epjconf/202327913002">10.1051/epjconf/202327913002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of a jet gas target system for the Felsenkeller underground accelerator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Yadav%2C+A">Anup Yadav</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">Konrad Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</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="2210.15218v1-abstract-short" style="display: inline;"> For direct cross-section measurements in nuclear astrophysics, in addition to suitable ion beams and detectors, also highly pure and stable targets are needed. Here, using a gas jet as a target offers an attractive approach that combines high stability even under significant beam load with excellent purity and high localisation. Such a target is currently under construction at the Felsenkeller und… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15218v1-abstract-full').style.display = 'inline'; document.getElementById('2210.15218v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.15218v1-abstract-full" style="display: none;"> For direct cross-section measurements in nuclear astrophysics, in addition to suitable ion beams and detectors, also highly pure and stable targets are needed. Here, using a gas jet as a target offers an attractive approach that combines high stability even under significant beam load with excellent purity and high localisation. Such a target is currently under construction at the Felsenkeller underground ion accelerator lab for nuclear astrophysics in Dresden, Germany. The target thickness will be measured by optical interferometry, allowing an in-situ thickness determination including also beam-induced effects. The contribution reports on the status of this new system and outlines possible applications in nuclear astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.15218v1-abstract-full').style.display = 'none'; document.getElementById('2210.15218v1-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> 27 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Submitted to Nuclear Physics in Astrophysics - X conference proceeding</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.03051">arXiv:2209.03051</a> <span> [<a href="https://arxiv.org/pdf/2209.03051">pdf</a>, <a href="https://arxiv.org/format/2209.03051">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/s10050-022-00827-2">10.1140/epja/s10050-022-00827-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First direct limit on the 334 keV resonance strength in the $^{22}$Ne(伪,纬)$^{26}$Mg reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Masha%2C+E">E. Masha</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Compagnucci%2C+A">A. Compagnucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=di+Leva%2C+A">A. di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a> , et al. (22 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="2209.03051v1-abstract-short" style="display: inline;"> In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with the emission of a neutron, or $^{26}$Mg and a $纬$ ray. At high temperature, the ($伪,n$) channel dominates, while at low temperature, it is energetically hampered. The rate of its competitor, the $^{22}$Ne($伪$,$纬$)$^{26}$Mg reaction, and, hence, the minimum temperature for the ($伪,n$) dominance, are controlled by many n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03051v1-abstract-full').style.display = 'inline'; document.getElementById('2209.03051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.03051v1-abstract-full" style="display: none;"> In stars, the fusion of $^{22}$Ne and $^4$He may produce either $^{25}$Mg, with the emission of a neutron, or $^{26}$Mg and a $纬$ ray. At high temperature, the ($伪,n$) channel dominates, while at low temperature, it is energetically hampered. The rate of its competitor, the $^{22}$Ne($伪$,$纬$)$^{26}$Mg reaction, and, hence, the minimum temperature for the ($伪,n$) dominance, are controlled by many nuclear resonances. The strengths of these resonances have hitherto been studied only indirectly. The present work aims to directly measure the total strength of the resonance at $E$_{r}$\,=\,$334$\,$keV (corresponding to $E$_{x}$\,=\,$10949$\,$keV in $^{26}$Mg). The data reported here have been obtained using high intensity $^4$He$^+$ beam from the INFN LUNA 400 kV underground accelerator, a windowless, recirculating, 99.9% isotopically enriched $^{22}$Ne gas target, and a 4$蟺$ bismuth germanate summing $纬$-ray detector. The ultra-low background rate of less than 0.5 counts/day was determined using 67 days of no-beam data and 7 days of $^4$He$^+$ beam on an inert argon target. The new high-sensitivity setup allowed to determine the first direct upper limit of 4.0$\,\times\,$10$^{-11}$ eV (at 90% confidence level) for the resonance strength. Finally, the sensitivity of this setup paves the way to study further $^{22}$Ne($伪$,$纬$)$^{26}$Mg resonances at higher energy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.03051v1-abstract-full').style.display = 'none'; document.getElementById('2209.03051v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Submitted to Eur. Phys. J. A</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 58, 194 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.14263">arXiv:2204.14263</a> <span> [<a href="https://arxiv.org/pdf/2204.14263">pdf</a>, <a href="https://arxiv.org/format/2204.14263">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 Physics - Experiment">hep-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/epjc/s10052-022-10755-6">10.1140/epjc/s10052-022-10755-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Long-term evolution of the neutron rate at the Canfranc Underground Laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Orrigo%2C+S+E+A">S. E. A. Orrigo</a>, <a href="/search/nucl-ex?searchtype=author&query=Tain%2C+J+L">J. L. Tain</a>, <a href="/search/nucl-ex?searchtype=author&query=Mont-Geli%2C+N">N. Mont-Geli</a>, <a href="/search/nucl-ex?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">A. Tarife帽o-Saldivia</a>, <a href="/search/nucl-ex?searchtype=author&query=Fraile%2C+L+M">L. M. Fraile</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Agramunt%2C+J">J. Agramunt</a>, <a href="/search/nucl-ex?searchtype=author&query=Algora%2C+A">A. Algora</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Calvi%C3%B1o%2C+F">F. Calvi帽o</a>, <a href="/search/nucl-ex?searchtype=author&query=Cort%C3%A9s%2C+G">G. Cort茅s</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Blas%2C+A">A. De Blas</a>, <a href="/search/nucl-ex?searchtype=author&query=Dillmann%2C+I">I. Dillmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Bugar%C3%ADn%2C+A+D">A. Dom铆nguez Bugar铆n</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+R">R. Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Nacher%2C+E">E. Nacher</a>, <a href="/search/nucl-ex?searchtype=author&query=Tolosa-Delgado%2C+A">A. Tolosa-Delgado</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="2204.14263v2-abstract-short" style="display: inline;"> We report results on the long-term variation of the neutron counting rate at the Canfranc Underground Laboratory, of importance for several low-background experiments installed there, including rare-event searches. The measurement campaign was performed employing the High Efficiency Neutron Spectrometry Array (HENSA) mounted in Hall A and lasted 412 live days. The present study is the first long-t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.14263v2-abstract-full').style.display = 'inline'; document.getElementById('2204.14263v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.14263v2-abstract-full" style="display: none;"> We report results on the long-term variation of the neutron counting rate at the Canfranc Underground Laboratory, of importance for several low-background experiments installed there, including rare-event searches. The measurement campaign was performed employing the High Efficiency Neutron Spectrometry Array (HENSA) mounted in Hall A and lasted 412 live days. The present study is the first long-term measurement of the neutron rate with sensitivity over a wide range of neutron energies (from thermal up to 0.1 GeV and beyond) performed in any underground laboratory so far. Data on the environmental variables inside the experimental hall (radon concentration, air temperature, air pressure and humidity) were also acquired during all the measurement campaign. We have investigated for the first time the evolution of the neutron rate for different energies of the neutrons and its correlation with the ambient variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.14263v2-abstract-full').style.display = 'none'; document.getElementById('2204.14263v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 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">12 pages, 5 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 82, 814 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.12616">arXiv:2111.12616</a> <span> [<a href="https://arxiv.org/pdf/2111.12616">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 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/10.1088/1742-6596/2156/1/012223">10.1088/1742-6596/2156/1/012223 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First results from the HENSA/ANAIS collaboration at the Canfranc Underground Laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Mont-Geli%2C+N">N Mont-Geli</a>, <a href="/search/nucl-ex?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">A Tarife帽o-Saldivia</a>, <a href="/search/nucl-ex?searchtype=author&query=Orrigo%2C+S+E+A">S E A Orrigo</a>, <a href="/search/nucl-ex?searchtype=author&query=Tain%2C+J+L">J L Tain</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Agramunt%2C+J">J Agramunt</a>, <a href="/search/nucl-ex?searchtype=author&query=Algora%2C+A">A Algora</a>, <a href="/search/nucl-ex?searchtype=author&query=Amar%C3%A9%2C+J">J Amar茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Calvi%C3%B1o%2C+F">F Calvi帽o</a>, <a href="/search/nucl-ex?searchtype=author&query=Cebri%C3%A1n%2C+S">S Cebri谩n</a>, <a href="/search/nucl-ex?searchtype=author&query=Coarasa%2C+I">I Coarasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Cort%C3%A9s%2C+G">G Cort茅s</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Blas%2C+A">A De Blas</a>, <a href="/search/nucl-ex?searchtype=author&query=Dillmann%2C+I">I Dillmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Fraile%2C+L+M">L M Fraile</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+E">E Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+R">R Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Mart%C3%ADnez%2C+M">M Mart铆nez</a>, <a href="/search/nucl-ex?searchtype=author&query=Nacher%2C+E">E Nacher</a>, <a href="/search/nucl-ex?searchtype=author&query=Ortigoza%2C+Y">Y Ortigoza</a>, <a href="/search/nucl-ex?searchtype=author&query=Ortiz%2C+A">A Ortiz</a>, <a href="/search/nucl-ex?searchtype=author&query=Pall%C3%A0s%2C+M">M Pall脿s</a>, <a href="/search/nucl-ex?searchtype=author&query=Puimed%C3%B3n%2C+J">J Puimed贸n</a>, <a href="/search/nucl-ex?searchtype=author&query=Salinas%2C+A">A Salinas</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="2111.12616v2-abstract-short" style="display: inline;"> The HENSA/ANAIS collaboration aims for the precise determination of the neutron flux that could affect ANAIS-112, an experiment looking for the dark matter annual modulation using NaI(Tl) scintillators. In this work, the first measurements of the neutron flux and Monte Carlo simulations of the neutron spectrum are reported. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.12616v2-abstract-full" style="display: none;"> The HENSA/ANAIS collaboration aims for the precise determination of the neutron flux that could affect ANAIS-112, an experiment looking for the dark matter annual modulation using NaI(Tl) scintillators. In this work, the first measurements of the neutron flux and Monte Carlo simulations of the neutron spectrum are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.12616v2-abstract-full').style.display = 'none'; document.getElementById('2111.12616v2-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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/2111.09202">arXiv:2111.09202</a> <span> [<a href="https://arxiv.org/pdf/2111.09202">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-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/10.1088/1742-6596/2156/1/012169">10.1088/1742-6596/2156/1/012169 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the neutron flux at the Canfranc Underground Laboratory with HENSA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Orrigo%2C+S+E+A">S. E. A. Orrigo</a>, <a href="/search/nucl-ex?searchtype=author&query=Tain%2C+J+L">J. L. Tain</a>, <a href="/search/nucl-ex?searchtype=author&query=Mont-Geli%2C+N">N. Mont-Geli</a>, <a href="/search/nucl-ex?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">A. Tarife帽o-Saldivia</a>, <a href="/search/nucl-ex?searchtype=author&query=Fraile%2C+L+M">L. M. Fraile</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Agramunt%2C+J">J. Agramunt</a>, <a href="/search/nucl-ex?searchtype=author&query=Algora%2C+A">A. Algora</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Calvi%C3%B1o%2C+F">F. Calvi帽o</a>, <a href="/search/nucl-ex?searchtype=author&query=Cort%C3%A9s%2C+G">G. Cort茅s</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Blas%2C+A">A. De Blas</a>, <a href="/search/nucl-ex?searchtype=author&query=Dillmann%2C+I">I. Dillmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Bugar%C3%ADn%2C+A+D">A. Dom铆nguez Bugar铆n</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+R">R. Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Nacher%2C+E">E. Nacher</a>, <a href="/search/nucl-ex?searchtype=author&query=Tolosa%2C+A">A. Tolosa</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="2111.09202v1-abstract-short" style="display: inline;"> We have performed a long-term measurement of the neutron flux with the High Efficiency Neutron Spectrometry Array HENSA in the Hall A of the Canfranc Underground Laboratory. The Hall A measurement campaign lasted from October 2019 to March 2021, demonstrating an excellent stability of the HENSA setup. Preliminary results on the neutron flux from this campaign are presented for the first time. In P… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09202v1-abstract-full').style.display = 'inline'; document.getElementById('2111.09202v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.09202v1-abstract-full" style="display: none;"> We have performed a long-term measurement of the neutron flux with the High Efficiency Neutron Spectrometry Array HENSA in the Hall A of the Canfranc Underground Laboratory. The Hall A measurement campaign lasted from October 2019 to March 2021, demonstrating an excellent stability of the HENSA setup. Preliminary results on the neutron flux from this campaign are presented for the first time. In Phase 1 (113 live days) a total neutron flux of 1.66(2) $\times$10$^{-5}$ cm$^{-2}$ s$^{-1}$ is obtained. Our results are in good agreement with those from our previous shorter measurement where a reduced experimental setup was employed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09202v1-abstract-full').style.display = 'none'; document.getElementById('2111.09202v1-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, 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">Proceedings of the 17th International Conference on Topics in Astroparticle and Underground Physics (TAUP 2021)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00303">arXiv:2110.00303</a> <span> [<a href="https://arxiv.org/pdf/2110.00303">pdf</a>, <a href="https://arxiv.org/format/2110.00303">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.127.152701">10.1103/PhysRevLett.127.152701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct measurement of the 13C(伪,n)16O cross section into the s-process Gamow peak </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapagnani%2C+D">D. Rapagnani</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Cristallo%2C+S">S. Cristallo</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=DiLeva%2C+A">A. DiLeva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E">E. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a> , et al. (23 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="2110.00303v1-abstract-short" style="display: inline;"> One of the main neutron sources for the astrophysical s-process is the reaction 13C(伪,n)16O, taking place in thermally pulsing Asymptotic Giant Branch stars at temperatures around 90 MK. To model the nucleosynthesis during this process the reaction cross section needs to be known in the 150-230keV energy window (Gamow peak). At these sub-Coulomb energies cross section direct measurements are sever… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00303v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00303v1-abstract-full" style="display: none;"> One of the main neutron sources for the astrophysical s-process is the reaction 13C(伪,n)16O, taking place in thermally pulsing Asymptotic Giant Branch stars at temperatures around 90 MK. To model the nucleosynthesis during this process the reaction cross section needs to be known in the 150-230keV energy window (Gamow peak). At these sub-Coulomb energies cross section direct measurements are severely affected by the low event rate, making us rely on input from indirect methods and extrapolations from higher-energy direct data. This leads to an uncertainty in the cross section at the relevant energies too high to reliably constrain the nuclear physics input to s-process calculations. We present the results from a new deep-underground measurement of 13C(伪,n)16O, covering the energy range 230-300keV, with drastically reduced uncertainties over previous measurements and for the first time providing data directly inside the s-process Gamow peak. Selected stellar models have been computed to estimate the impact of our revised reaction rate. For stars of nearly solar composition, we find sizeable variations of some isotopes, whose production is influenced by the activation of close-by branching points that are sensitive to the neutron density, in particular the two radioactive nuclei 60Fe and 205Pb, as well as 152Gd <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00303v1-abstract-full').style.display = 'none'; document.getElementById('2110.00303v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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, accepted on PRL on 17th August 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.08613">arXiv:2107.08613</a> <span> [<a href="https://arxiv.org/pdf/2107.08613">pdf</a>, <a href="https://arxiv.org/format/2107.08613">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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="High Energy Physics - Experiment">hep-ex</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/10.1146/annurev-nucl-011921-061243">10.1146/annurev-nucl-011921-061243 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Future of Solar Neutrinos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Gann%2C+G+D+O">G. D. Orebi Gann</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Serenelli%2C+A">A. Serenelli</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="2107.08613v1-abstract-short" style="display: inline;"> In this article we review the current state of the field of solar neutrinos, including flavour oscillations, non-standard effects, solar models, cross section measurements, and the broad experimental program thus motivated and enabled. We discuss the historical discoveries that contributed to current knowledge, and define critical open questions to be addressed in the next decade. We discuss the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08613v1-abstract-full').style.display = 'inline'; document.getElementById('2107.08613v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.08613v1-abstract-full" style="display: none;"> In this article we review the current state of the field of solar neutrinos, including flavour oscillations, non-standard effects, solar models, cross section measurements, and the broad experimental program thus motivated and enabled. We discuss the historical discoveries that contributed to current knowledge, and define critical open questions to be addressed in the next decade. We discuss the state of the art of standard solar models, including uncertainties and problems related to the solar composition, and review experimental and model solar neutrino fluxes, including future prospects. We review the state of the art of the nuclear reaction data relevant for solar fusion in the proton-proton chain and carbon-nitrogen-oxygen cycle. Finally, we review the current and future experimental program that can address outstanding questions in this field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.08613v1-abstract-full').style.display = 'none'; document.getElementById('2107.08613v1-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 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> Annual Review of Nuclear and Particle Science 71, 491-528 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.12214">arXiv:2106.12214</a> <span> [<a href="https://arxiv.org/pdf/2106.12214">pdf</a>, <a href="https://arxiv.org/ps/2106.12214">ps</a>, <a href="https://arxiv.org/format/2106.12214">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.105.024303">10.1103/PhysRevC.105.024303 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photoexcitation of $^{76}$Ge </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=Massarczyk%2C+R">R. Massarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</a>, <a href="/search/nucl-ex?searchtype=author&query=Beyer%2C+R">R. Beyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammer%2C+S">S. Hammer</a>, <a href="/search/nucl-ex?searchtype=author&query=Hartmann%2C+A">A. Hartmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">T. Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Hoffmann%2C+H+F">H. F. Hoffmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">A. R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=K%C3%B6gler%2C+T">T. K枚gler</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S+E">S. E. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Pichotta%2C+M">M. Pichotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Turkat%2C+S">S. Turkat</a>, <a href="/search/nucl-ex?searchtype=author&query=Turko%2C+J+A+B">J. A. B. Turko</a>, <a href="/search/nucl-ex?searchtype=author&query=Urla%C3%9F%2C+S">S. Urla脽</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</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="2106.12214v2-abstract-short" style="display: inline;"> The dipole strength of the nuclide $^{76}$Ge was studied in photon-scattering experiments using bremsstrahlung produced with electron beams of energies of 7.8 and 12.3 MeV at the $纬$ELBE facility. We identified 210 levels up to an excitation energy of 9.4 MeV and assigned spin $J$ = 1 to most of them. The quasicontinuum of unresolved transitions was included in the analysis of the spectra and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12214v2-abstract-full').style.display = 'inline'; document.getElementById('2106.12214v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.12214v2-abstract-full" style="display: none;"> The dipole strength of the nuclide $^{76}$Ge was studied in photon-scattering experiments using bremsstrahlung produced with electron beams of energies of 7.8 and 12.3 MeV at the $纬$ELBE facility. We identified 210 levels up to an excitation energy of 9.4 MeV and assigned spin $J$ = 1 to most of them. The quasicontinuum of unresolved transitions was included in the analysis of the spectra and the intensities of branching transitions were estimated on the basis of simulations of statistical $纬$-ray cascades. The photoabsorption cross section up to the neutron-separation energy was determined and is compared with predictions of the statistical reaction model. The derived photon strength function is compared with results of experiments using other reactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12214v2-abstract-full').style.display = 'none'; document.getElementById('2106.12214v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">12 pages, 9 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/2104.06914">arXiv:2104.06914</a> <span> [<a href="https://arxiv.org/pdf/2104.06914">pdf</a>, <a href="https://arxiv.org/format/2104.06914">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.103.045805">10.1103/PhysRevC.103.045805 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the $^{2}$H($p,纬$)$^{3}$He S-factor at 265-1094keV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Turkat%2C+S">S. Turkat</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammer%2C+S">S. Hammer</a>, <a href="/search/nucl-ex?searchtype=author&query=Masha%2C+E">E. Masha</a>, <a href="/search/nucl-ex?searchtype=author&query=Akhmadaliev%2C+S">S. Akhmadaliev</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">T. Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Julin%2C+J">J. Julin</a>, <a href="/search/nucl-ex?searchtype=author&query=Koppitz%2C+M">M. Koppitz</a>, <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">F. Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%B6ckel%2C+C">C. M枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">S. Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="2104.06914v1-abstract-short" style="display: inline;"> Recent astronomical data have provided the primordial deuterium abundance with percent precision. As a result, Big Bang nucleosynthesis may provide a constraint on the universal baryon to photon ratio that is as precise as, but independent from, analyses of the cosmic microwave background. However, such a constraint requires that the nuclear reaction rates governing the production and destruction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.06914v1-abstract-full').style.display = 'inline'; document.getElementById('2104.06914v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.06914v1-abstract-full" style="display: none;"> Recent astronomical data have provided the primordial deuterium abundance with percent precision. As a result, Big Bang nucleosynthesis may provide a constraint on the universal baryon to photon ratio that is as precise as, but independent from, analyses of the cosmic microwave background. However, such a constraint requires that the nuclear reaction rates governing the production and destruction of primordial deuterium are sufficiently well known. Here, a new measurement of the $^2$H($p,纬$)$^3$He cross section is reported. This nuclear reaction dominates the error on the predicted Big Bang deuterium abundance. A proton beam of 400-1650keV beam energy was incident on solid titanium deuteride targets, and the emitted $纬$-rays were detected in two high-purity germanium detectors at angles of 55$^\circ$ and 90$^\circ$, respectively. The deuterium content of the targets has been obtained in situ by the $^2$H($^3$He,$p$)$^4$He reaction and offline using the Elastic Recoil Detection method. The astrophysical S-factor has been determined at center of mass energies between 265 and 1094 keV, addressing the uppermost part of the relevant energy range for Big Bang nucleosynthesis and complementary to ongoing work at lower energies. The new data support a higher S-factor at Big Bang temperatures than previously assumed, reducing the predicted deuterium abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.06914v1-abstract-full').style.display = 'none'; document.getElementById('2104.06914v1-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 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, 9 figures, 4 tables; to be published in 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 103, 045805 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.02696">arXiv:2006.02696</a> <span> [<a href="https://arxiv.org/pdf/2006.02696">pdf</a>, <a href="https://arxiv.org/format/2006.02696">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="High Energy Physics - Experiment">hep-ex</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/PhysRevD.101.123027">10.1103/PhysRevD.101.123027 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron flux and spectrum in the Dresden Felsenkeller underground facility studied by moderated $^3$He counters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">T. Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Agramunt%2C+J">J. Agramunt</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Degering%2C+D">D. Degering</a>, <a href="/search/nucl-ex?searchtype=author&query=Dillmann%2C+I">I. Dillmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Fraile%2C+L+M">L. M. Fraile</a>, <a href="/search/nucl-ex?searchtype=author&query=Jordan%2C+D">D. Jordan</a>, <a href="/search/nucl-ex?searchtype=author&query=K%C3%B6ster%2C+U">U. K枚ster</a>, <a href="/search/nucl-ex?searchtype=author&query=Marta%2C+M">M. Marta</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S+E">S. E. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Ta%C3%ADn%2C+J+L">J. L. Ta铆n</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="2006.02696v2-abstract-short" style="display: inline;"> Ambient neutrons may cause significant background for underground experiments. Therefore, it is necessary to investigate their flux and energy spectrum in order to devise a proper shielding. Here, two sets of altogether ten moderated $^3$He neutron counters are used for a detailed study of the ambient neutron background in tunnel IV of the Felsenkeller facility, underground below 45 meters of rock… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02696v2-abstract-full').style.display = 'inline'; document.getElementById('2006.02696v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.02696v2-abstract-full" style="display: none;"> Ambient neutrons may cause significant background for underground experiments. Therefore, it is necessary to investigate their flux and energy spectrum in order to devise a proper shielding. Here, two sets of altogether ten moderated $^3$He neutron counters are used for a detailed study of the ambient neutron background in tunnel IV of the Felsenkeller facility, underground below 45 meters of rock in Dresden/Germany. One of the moderators is lined with lead and thus sensitive to neutrons of energies higher than 10 MeV. For each $^3$He counter-moderator assembly, the energy dependent neutron sensitivity was calculated with the FLUKA code. The count rates of the ten detectors were then fitted with the MAXED and GRAVEL packages. As a result, both the neutron energy spectrum from 10$^{-9}$ MeV to 300 MeV and the flux integrated over the same energy range were determined experimentally. The data show that at a given depth, both the flux and the spectrum vary significantly depending on local conditions. Energy integrated fluxes of $(0.61 \pm 0.05)$, $(1.96 \pm 0.15)$, and $(4.6 \pm 0.4) \times 10^{-4}$ cm$^{-2}$ s$^{-1}$, respectively, are measured for three sites within Felsenkeller tunnel IV which have similar muon flux but different shielding wall configurations. The integrated neutron flux data and the obtained spectra for the three sites are matched reasonably well by FLUKA Monte Carlo calculations that are based on the known muon flux and composition of the measurement room walls. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02696v2-abstract-full').style.display = 'none'; document.getElementById('2006.02696v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">Comments:</span> <span class="has-text-grey-dark mathjax">10 figures, 4 tables; to be published in Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 123027 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.00002">arXiv:2005.00002</a> <span> [<a href="https://arxiv.org/pdf/2005.00002">pdf</a>, <a href="https://arxiv.org/format/2005.00002">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1140/epja/s10050-020-00149-1">10.1140/epja/s10050-020-00149-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Setup commissioning for an improved measurement of the D(p,gamma)3He cross section at Big Bang Nucleosynthesis energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a> , et al. (22 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="2005.00002v1-abstract-short" style="display: inline;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'inline'; document.getElementById('2005.00002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.00002v1-abstract-full" style="display: none;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3He reaction at the Laboratory for Underground Nuclear Astrophysics of the Gran Sasso Laboratory (Italy). The commissioning was aimed at minimising all sources of systematic uncertainty in the measured cross sections. The overall systematic error achieved (< 3 %) will enable improved predictions of BBN deuterium abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'none'; document.getElementById('2005.00002v1-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 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">11 pages, 11 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/2001.08744">arXiv:2001.08744</a> <span> [<a href="https://arxiv.org/pdf/2001.08744">pdf</a>, <a href="https://arxiv.org/ps/2001.08744">ps</a>, <a href="https://arxiv.org/format/2001.08744">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/10.1140/epja/s10050-020-00077-0">10.1140/epja/s10050-020-00077-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new approach to monitor 13C-targets degradation in situ for 13C(alpha,n)16O cross-section measurements at LUNA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Paolo%2C+L">L. Di Paolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</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="2001.08744v2-abstract-short" style="display: inline;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section resu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08744v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08744v2-abstract-full" style="display: none;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section results. A common technique used for these purposes is the Nuclear Resonant Reaction Analysis (NRRA), which however requires that a narrow resonance be available inside the dynamic range of the accelerator used. In cases when this is not possible, as for example the 13C(alpha,n)16O reaction recently studied at low energies at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy, alternative approaches must be found. Here, we present a new application of the shape analysis of primary gamma rays emitted by the 13C(p,g)14N radiative capture reaction. This approach was used to monitor 13C target degradation {\em in situ} during the 13C(alpha,n)16O data taking campaign. The results obtained are in agreement with evaluations subsequently performed at Atomki (Hungary) using the NRRA method. A preliminary application for the extraction of the 13C(alpha,n)16O reaction cross-section at one beam energy is also reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'none'; document.getElementById('2001.08744v2-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">10 pages, 6 figures, to be published in EPJ A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The European Physical Journal A volume 56, Article number: 75 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.08945">arXiv:1908.08945</a> <span> [<a href="https://arxiv.org/pdf/1908.08945">pdf</a>, <a href="https://arxiv.org/format/1908.08945">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="Instrumentation and Detectors">physics.ins-det</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/i2019-12865-4">10.1140/epja/i2019-12865-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Background in $纬$-ray detectors and carbon beam tests in the Felsenkeller shallow-underground accelerator laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Degering%2C+D">D. Degering</a>, <a href="/search/nucl-ex?searchtype=author&query=Domula%2C+A">A. Domula</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">F. Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Steckling%2C+J">J. Steckling</a>, <a href="/search/nucl-ex?searchtype=author&query=Turkat%2C+S">S. Turkat</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1908.08945v1-abstract-short" style="display: inline;"> The relevant interaction energies for astrophysical radiative capture reactions are very low, much below the repulsive Coulomb barrier. This leads to low cross sections, low counting rates in $纬$-ray detectors, and therefore the need to perform such experiments at ion accelerators placed in underground settings, shielded from cosmic rays. Here, the feasibility of such experiments in the new shallo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08945v1-abstract-full').style.display = 'inline'; document.getElementById('1908.08945v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.08945v1-abstract-full" style="display: none;"> The relevant interaction energies for astrophysical radiative capture reactions are very low, much below the repulsive Coulomb barrier. This leads to low cross sections, low counting rates in $纬$-ray detectors, and therefore the need to perform such experiments at ion accelerators placed in underground settings, shielded from cosmic rays. Here, the feasibility of such experiments in the new shallow-underground accelerator laboratory in tunnels VIII and IX of the Felsenkeller site in Dresden, Germany, is evaluated. To this end, the no-beam background in three different types of germanium detectors, i.e. a Euroball/Miniball triple cluster and two large monolithic detectors, is measured over periods of 26-66 days. The cosmic-ray induced background is found to be reduced by a factor of 500-2400, by the combined effects of, first, the 140 meters water equivalent overburden attenuating the cosmic muon flux by a factor of 40, and second, scintillation veto detectors gating out most of the remaining muon-induced effects. The new background data are compared to spectra taken with the same detectors at the Earth's surface and at other underground sites. Subsequently, the beam intensity from the cesium sputter ion source installed in Felsenkeller has been studied over periods of several hours. Based on the background and beam intensity data reported here, for the example of the $^{12}$C($伪$,$纬$)$^{16}$O reaction it is shown that highly sensitive experiments will be possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.08945v1-abstract-full').style.display = 'none'; document.getElementById('1908.08945v1-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 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </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 to Eur. Phys. J. A</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 55, 174 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.11501">arXiv:1904.11501</a> <span> [<a href="https://arxiv.org/pdf/1904.11501">pdf</a>, <a href="https://arxiv.org/format/1904.11501">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.astropartphys.2019.04.006">10.1016/j.astropartphys.2019.04.006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The muon intensity in the Felsenkeller shallow underground laboratory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">F. Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Al-Abdullah%2C+T">T. Al-Abdullah</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnaf%C3%B6ldi%2C+G+G">G. G. Barnaf枚ldi</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Degering%2C+D">D. Degering</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Sur%C3%A1nyi%2C+G">G. Sur谩nyi</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1904.11501v1-abstract-short" style="display: inline;"> The muon intensity and angular distribution in the shallow-underground laboratory Felsenkeller in Dresden, Germany have been studied using a portable muon detector based on the close cathode chamber design. Data has been taken at four positions in Felsenkeller tunnels VIII and IX, where a new 5 MV underground ion accelerator is being installed, and in addition at four positions in Felsenkeller tun… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11501v1-abstract-full').style.display = 'inline'; document.getElementById('1904.11501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.11501v1-abstract-full" style="display: none;"> The muon intensity and angular distribution in the shallow-underground laboratory Felsenkeller in Dresden, Germany have been studied using a portable muon detector based on the close cathode chamber design. Data has been taken at four positions in Felsenkeller tunnels VIII and IX, where a new 5 MV underground ion accelerator is being installed, and in addition at four positions in Felsenkeller tunnel IV, which hosts a low-radioactivity counting facility. At each of the eight positions studied, seven different orientations of the detector were used to compile a map of the upper hemisphere with 0.85掳 angular resolution. The muon intensity is found to be suppressed by a factor of 40 due to the 45 m thick rock overburden, corresponding to 140 meters water equivalent. The angular data are matched by two different simulations taking into account the known geodetic features of the terrain: First, simply by determining the cutoff energy using the projected slant depth in rock and the known muon energy spectrum, and second, in a Geant4 simulation propagating the muons through a column of rock equal to the known slant depth. The present data are instrumental for studying muon-induced effects at these depths and also in the planning of an active veto for accelerator-based underground nuclear astrophysics experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11501v1-abstract-full').style.display = 'none'; document.getElementById('1904.11501v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </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 to Astroparticle Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 112 (2019) 24-34 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.08201">arXiv:1810.08201</a> <span> [<a href="https://arxiv.org/pdf/1810.08201">pdf</a>, <a href="https://arxiv.org/format/1810.08201">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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/10.1142/9789811204296_0015">10.1142/9789811204296_0015 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The new Felsenkeller 5 MV underground accelerator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cowan%2C+T+E">Thomas E. Cowan</a>, <a href="/search/nucl-ex?searchtype=author&query=Domula%2C+A">Alexander Domula</a>, <a href="/search/nucl-ex?searchtype=author&query=D%C3%B6ring%2C+T">Toralf D枚ring</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">Marcel Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammer%2C+S">Sebastian Hammer</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">Thomas Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=H%C3%BCbinger%2C+L">Lisa H眉binger</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">Arnd R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">Felix Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S+E">Stefan E. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">Stefan Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Rimarzig%2C+B">Bernd Rimarzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">Konrad Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">Ronald Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">Klaus St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">Tam谩s Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Turkat%2C+S">Steffen Turkat</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">Andreas Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">Louis Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="1810.08201v2-abstract-short" style="display: inline;"> The field of nuclear astrophysics is devoted to the study of the creation of the chemical elements. By nature, it is deeply intertwined with the physics of the Sun. The nuclear reactions of the proton-proton cycle of hydrogen burning, including the 3He(伪,纬)7Be reaction, provide the necessary nuclear energy to prevent the gravitational collapse of the Sun and give rise to the by now well-studied pp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.08201v2-abstract-full').style.display = 'inline'; document.getElementById('1810.08201v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.08201v2-abstract-full" style="display: none;"> The field of nuclear astrophysics is devoted to the study of the creation of the chemical elements. By nature, it is deeply intertwined with the physics of the Sun. The nuclear reactions of the proton-proton cycle of hydrogen burning, including the 3He(伪,纬)7Be reaction, provide the necessary nuclear energy to prevent the gravitational collapse of the Sun and give rise to the by now well-studied pp, 7Be, and 8B solar neutrinos. The not yet measured flux of 13N, 15O, and 17F neutrinos from the carbon-nitrogen-oxygen cycle is affected in rate by the 14N(p,纬)15O reaction and in emission profile by the 12C(p,纬)13N reaction. The nucleosynthetic output of the subsequent phase in stellar evolution, helium burning, is controlled by the 12C(伪,纬)16O reaction. In order to properly interpret the existing and upcoming solar neutrino data, precise nuclear physics information is needed. For nuclear reactions between light, stable nuclei, the best available technique are experiments with small ion accelerators in underground, low-background settings. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso/Italy, using a 0.4 MV accelerator. The present contribution reports on a higher-energy, 5.0 MV, underground accelerator in the Felsenkeller underground site in Dresden/Germany. Results from 纬-ray, neutron, and muon background measurements in the Felsenkeller underground site in Dresden, Germany, show that the background conditions are satisfactory for nuclear astrophysics purposes. The accelerator is in the commissioning phase and will provide intense, up to 50渭A, beams of 1H+, 4He+ , and 12C+ ions, enabling research on astrophysically relevant nuclear reactions with unprecedented sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.08201v2-abstract-full').style.display = 'none'; document.getElementById('1810.08201v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 to the Proceedings of the 5th International Solar Neutrino Conference, Dresden/Germany, 11-14 June 2018, to appear on World Scientific -- updated version (Figure 2 and relevant discussion updated, co-author A. Domula added)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.01628">arXiv:1810.01628</a> <span> [<a href="https://arxiv.org/pdf/1810.01628">pdf</a>, <a href="https://arxiv.org/format/1810.01628">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.121.172701">10.1103/PhysRevLett.121.172701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct capture cross section and the $E_p$ = 71 and 105 keV resonances in the $^{22}$Ne($p,纬$)$^{23}$Na reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Erasmo%2C+G">G. D'Erasmo</a>, <a href="/search/nucl-ex?searchtype=author&query=DiLeva%2C+A">A. DiLeva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a> , et al. (19 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="1810.01628v1-abstract-short" style="display: inline;"> The $^{22}$Ne($p,纬$)$^{23}$Na reaction, part of the neon-sodium cycle of hydrogen burning, may explain the observed anticorrelation between sodium and oxygen abundances in globular cluster stars. Its rate is controlled by a number of low-energy resonances and a slowly varying non-resonant component. Three new resonances at $E_p$ = 156.2, 189.5, and 259.7 keV have recently been observed and confirm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.01628v1-abstract-full').style.display = 'inline'; document.getElementById('1810.01628v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.01628v1-abstract-full" style="display: none;"> The $^{22}$Ne($p,纬$)$^{23}$Na reaction, part of the neon-sodium cycle of hydrogen burning, may explain the observed anticorrelation between sodium and oxygen abundances in globular cluster stars. Its rate is controlled by a number of low-energy resonances and a slowly varying non-resonant component. Three new resonances at $E_p$ = 156.2, 189.5, and 259.7 keV have recently been observed and confirmed. However, significant uncertainty on the reaction rate remains due to the non-resonant process and to two suggested resonances at $E_p$ = 71 and 105 keV. Here, new $^{22}$Ne($p,纬$)$^{23}$Na data with high statistics and low background are reported. Stringent upper limits of 6$\times$10$^{-11}$ and 7$\times$10$^{-11}$\,eV (90\% confidence level), respectively, are placed on the two suggested resonances. In addition, the off-resonant S-factor has been measured at unprecedented low energy, constraining the contributions from a subthreshold resonance and the direct capture process. As a result, at a temperature of 0.1 GK the error bar of the $^{22}$Ne($p,纬$)$^{23}$Na rate is now reduced by three orders of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.01628v1-abstract-full').style.display = 'none'; document.getElementById('1810.01628v1-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 October, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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 to Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 121, 172701 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.11501">arXiv:1806.11501</a> <span> [<a href="https://arxiv.org/pdf/1806.11501">pdf</a>, <a href="https://arxiv.org/format/1806.11501">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/10.1209/0295-5075/122/52001">10.1209/0295-5075/122/52001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effect of beam energy straggling on resonant yield in thin gas targets: The cases $^{22}$Ne(p,纬)$^{23}$Na and $^{14}$N(p,纬)$^{15}$O </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C">C. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/nucl-ex?searchtype=author&query=Gy%C3%BCrky%2C+G">Gy. Gy眉rky</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/nucl-ex?searchtype=author&query=Pantaleo%2C+F+R">F. R. Pantaleo</a>, <a href="/search/nucl-ex?searchtype=author&query=Prati%2C+P">P. Prati</a>, <a href="/search/nucl-ex?searchtype=author&query=Scott%2C+D+A">D. A. Scott</a>, <a href="/search/nucl-ex?searchtype=author&query=Straniero%2C+O">O. Straniero</a> , et al. (3 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="1806.11501v1-abstract-short" style="display: inline;"> When deriving resonance strengths using the thick-target yield approximation, for very narrow resonances it may be necessary to take beam energy straggling into account. This applies to gas targets of a few keV width, especially if there is some additional structure in target stoichiometry or detection efficiency. The correction for this effect is shown and tested on recent studies of narrow reson… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.11501v1-abstract-full').style.display = 'inline'; document.getElementById('1806.11501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.11501v1-abstract-full" style="display: none;"> When deriving resonance strengths using the thick-target yield approximation, for very narrow resonances it may be necessary to take beam energy straggling into account. This applies to gas targets of a few keV width, especially if there is some additional structure in target stoichiometry or detection efficiency. The correction for this effect is shown and tested on recent studies of narrow resonances in the $^{22}$Ne(p,纬)$^{23}$Na and $^{14}$N(p,纬)$^{15}$O reactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.11501v1-abstract-full').style.display = 'none'; document.getElementById('1806.11501v1-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 to Europhys. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Europhys. Lett. 122 (2018) 52001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.04777">arXiv:1803.04777</a> <span> [<a href="https://arxiv.org/pdf/1803.04777">pdf</a>, <a href="https://arxiv.org/ps/1803.04777">ps</a>, <a href="https://arxiv.org/format/1803.04777">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.120.152504">10.1103/PhysRevLett.120.152504 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strong neutron pairing in core+4n nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Revel%2C+A">A. Revel</a>, <a href="/search/nucl-ex?searchtype=author&query=Marques%2C+F+M">F. M. Marques</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Aumann%2C+T">T. Aumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">C. Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Holl%2C+M">M. Holl</a>, <a href="/search/nucl-ex?searchtype=author&query=Panin%2C+V">V. Panin</a>, <a href="/search/nucl-ex?searchtype=author&query=Vandebrouck%2C+M">M. Vandebrouck</a>, <a href="/search/nucl-ex?searchtype=author&query=Wamers%2C+F">F. Wamers</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=Atar%2C+L">L. Atar</a>, <a href="/search/nucl-ex?searchtype=author&query=Avdeichikov%2C+V">V. Avdeichikov</a>, <a href="/search/nucl-ex?searchtype=author&query=Beceiro-Novo%2C+S">S. Beceiro-Novo</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">J. Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C+A">C. A. Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Boillos%2C+J+M">J. M. Boillos</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Borge%2C+M+J+G">M. J. G. Borge</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">E. Casarejos</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=Cederk%C3%A4ll%2C+J">J. Cederk盲ll</a>, <a href="/search/nucl-ex?searchtype=author&query=Chartier%2C+M">M. Chartier</a>, <a href="/search/nucl-ex?searchtype=author&query=Chulkov%2C+L">L. Chulkov</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="1803.04777v1-abstract-short" style="display: inline;"> The emission of neutron pairs from the neutron-rich $N\!=\!12$ isotones $^{18}$C and $^{20}$O has been studied by high-energy nucleon knockout from $^{19}$N and $^{21}$O secondary beams, populating unbound states of the two isotones up to 15~MeV above their two-neutron emission thresholds. The analysis of triple fragment-$n$-$n$ correlations shows that the decay $^{19}$N$(-1p)^{18}$C… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.04777v1-abstract-full').style.display = 'inline'; document.getElementById('1803.04777v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.04777v1-abstract-full" style="display: none;"> The emission of neutron pairs from the neutron-rich $N\!=\!12$ isotones $^{18}$C and $^{20}$O has been studied by high-energy nucleon knockout from $^{19}$N and $^{21}$O secondary beams, populating unbound states of the two isotones up to 15~MeV above their two-neutron emission thresholds. The analysis of triple fragment-$n$-$n$ correlations shows that the decay $^{19}$N$(-1p)^{18}$C$^*\!\rightarrow^{16}$C+$n$+$n$ is clearly dominated by direct pair emission. The two-neutron correlation strength, the largest ever observed, suggests the predominance of a $^{14}$C core surrounded by four valence neutrons arranged in strongly correlated pairs. On the other hand, a significant competition of a sequential branch is found in the decay $^{21}$O$(-1n)^{20}$O$^*\!\rightarrow^{18}$O+$n$+$n$, attributed to its formation through the knockout of a deeply-bound neutron that breaks the $^{16}$O core and reduces the number of pairs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.04777v1-abstract-full').style.display = 'none'; document.getElementById('1803.04777v1-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 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">6 pages, 4 figures, accepted for publication in Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 120, 152504 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.04164">arXiv:1802.04164</a> <span> [<a href="https://arxiv.org/pdf/1802.04164">pdf</a>, <a href="https://arxiv.org/format/1802.04164">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/i2018-12476-7">10.1140/epja/i2018-12476-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-efficiency gas target setup for underground experiments, and redetermination of the branching ratio of the 189.5 keV $\mathbf{^{22}Ne(p,纬)^{23}Na}$ resonance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Erasmo%2C+G">G. D'Erasmo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a> , et al. (20 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="1802.04164v1-abstract-short" style="display: inline;"> The experimental study of nuclear reactions of astrophysical interest is greatly facilitated by a low-background, high-luminosity setup. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator offers ultra-low cosmic-ray induced background due to its location deep underground in the Gran Sasso National Laboratory (INFN-LNGS), Italy, and high intensity, 250-500 $渭$A, proton an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04164v1-abstract-full').style.display = 'inline'; document.getElementById('1802.04164v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.04164v1-abstract-full" style="display: none;"> The experimental study of nuclear reactions of astrophysical interest is greatly facilitated by a low-background, high-luminosity setup. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator offers ultra-low cosmic-ray induced background due to its location deep underground in the Gran Sasso National Laboratory (INFN-LNGS), Italy, and high intensity, 250-500 $渭$A, proton and $伪$ ion beams. In order to fully exploit these features, a high-purity, recirculating gas target system for isotopically enriched gases is coupled to a high-efficiency, six-fold optically segmented bismuth germanate (BGO) $纬$-ray detector. The beam intensity is measured with a beam calorimeter with constant temperature gradient. Pressure and temperature measurements have been carried out at several positions along the beam path, and the resultant gas density profile has been determined. Calibrated $纬$-intensity standards and the well-known $E_p$ = 278 keV $\mathrm{^{14}N(p,纬)^{15}O}$ resonance were used to determine the $纬$-ray detection efficiency and to validate the simulation of the target and detector setup. As an example, the recently measured resonance at $E_p$ = 189.5 keV in the $^{22}$Ne(p,$纬$)$^{23}$Na reaction has been investigated with high statistics, and the $纬$-decay branching ratios of the resonance have been determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04164v1-abstract-full').style.display = 'none'; document.getElementById('1802.04164v1-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 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">11 pages, 11 figures, accepted in Eur. Phys. Journal A</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 (2018) 54: 44 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.10847">arXiv:1711.10847</a> <span> [<a href="https://arxiv.org/pdf/1711.10847">pdf</a>, <a href="https://arxiv.org/format/1711.10847">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.97.015801">10.1103/PhysRevC.97.015801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Astrophysical S-factor of the $^{14}\textrm{N(p,}纬\textrm{)}^{15}\textrm{O}$ reaction at 0.4 -- 1.3\,MeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Akhmadaliev%2C+S">S. Akhmadaliev</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Gohl%2C+S">St. Gohl</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A">A. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Marta%2C+M">M. Marta</a>, <a href="/search/nucl-ex?searchtype=author&query=Munnik%2C+F">F. Munnik</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">T. P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">S. Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6der%2C+M">M. R枚der</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=Serfling%2C+M">M. Serfling</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Vomiero%2C+A">A. Vomiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1711.10847v1-abstract-short" style="display: inline;"> The $^{14}\textrm{N(p,}纬\textrm{)}^{15}\textrm{O}$ reaction is the slowest reaction of the carbon-nitrogen cycle of hydrogen burning and thus determines its rate. The precise knowledge of its rate is required to correctly model hydrogen burning in asymptotic giant branch stars. In addition, it is a necessary ingredient for a possible solution of the solar abundance problem by using the solar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10847v1-abstract-full').style.display = 'inline'; document.getElementById('1711.10847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.10847v1-abstract-full" style="display: none;"> The $^{14}\textrm{N(p,}纬\textrm{)}^{15}\textrm{O}$ reaction is the slowest reaction of the carbon-nitrogen cycle of hydrogen burning and thus determines its rate. The precise knowledge of its rate is required to correctly model hydrogen burning in asymptotic giant branch stars. In addition, it is a necessary ingredient for a possible solution of the solar abundance problem by using the solar $^{13}$N and $^{15}$O neutrino fluxes as probes of the carbon and nitrogen abundances in the solar core. After the downward revision of its cross section due to a much lower contribution by one particular transition, capture to the ground state in $^{15}$O, the evaluated total uncertainty is still 8\%, in part due to an unsatisfactory knowledge of the excitation function over a wide energy range. The present work reports precise S-factor data at twelve energies between 0.357-1.292~MeV for the strongest transition, capture to the 6.79~MeV excited state in $^{15}$O, and at ten energies between 0.479-1.202~MeV for the second strongest transition, capture to the ground state in $^{15}$O. An R-matrix fit is performed to estimate the impact of the new data on astrophysical energies. The recently suggested slight enhancement of the 6.79~MeV transition at low energy could not be confirmed. The present extrapolated zero-energy S-factors are $S_{6.79}(0)$~=~1.24$\pm$0.11~keV~barn and $S_{\rm GS}(0)$~=~0.19$\pm$0.05~keV~barn. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.10847v1-abstract-full').style.display = 'none'; document.getElementById('1711.10847v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </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 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 97, 015801 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.05033">arXiv:1711.05033</a> <span> [<a href="https://arxiv.org/pdf/1711.05033">pdf</a>, <a href="https://arxiv.org/format/1711.05033">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/10.1016/j.nuclphysa.2017.11.009">10.1016/j.nuclphysa.2017.11.009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the $^7$Be($p,纬$)$^8$B $S$-factor with the new precise $^7$Be solar neutrino flux from Borexino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">Marcell P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">Arnd R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="1711.05033v1-abstract-short" style="display: inline;"> Among the solar fusion reactions, the rate of the $^7$Be($p,纬$)$^8$B reaction is one of the most difficult to determine rates. In a number of previous experiments, its astrophysical $S$-factor has been measured at $E$ = 0.1-2.5 MeV center-of-mass energy. However, no experimental data is available below 0.1 MeV. Thus, an extrapolation to solar energies is necessary, resulting in significant uncerta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.05033v1-abstract-full').style.display = 'inline'; document.getElementById('1711.05033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.05033v1-abstract-full" style="display: none;"> Among the solar fusion reactions, the rate of the $^7$Be($p,纬$)$^8$B reaction is one of the most difficult to determine rates. In a number of previous experiments, its astrophysical $S$-factor has been measured at $E$ = 0.1-2.5 MeV center-of-mass energy. However, no experimental data is available below 0.1 MeV. Thus, an extrapolation to solar energies is necessary, resulting in significant uncertainty for the extrapolated $S$-factor. On the other hand, the measured solar neutrino fluxes are now very precise. Therefore, the problem of the $S$-factor determination is turned around here: Using the measured $^7$Be and $^8$B neutrino fluxes and the Standard Solar Model, the $^7$Be($p,纬$)$^8$B astrophysical $S$-factor is determined at the solar Gamow peak. In addition, the $^3$He($伪$,$纬$)$^7$Be $S$-factor is redetermined with a similar method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.05033v1-abstract-full').style.display = 'none'; document.getElementById('1711.05033v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </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 to Nucl. Phys. A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.07995">arXiv:1707.07995</a> <span> [<a href="https://arxiv.org/pdf/1707.07995">pdf</a>, <a href="https://arxiv.org/format/1707.07995">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.96.054305">10.1103/PhysRevC.96.054305 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effective proton-neutron interaction near the drip line from unbound states in $^{25,26}$F </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Vandebrouck%2C+M">M. Vandebrouck</a>, <a href="/search/nucl-ex?searchtype=author&query=Lepailleur%2C+A">A. Lepailleur</a>, <a href="/search/nucl-ex?searchtype=author&query=Sorlin%2C+O">O. Sorlin</a>, <a href="/search/nucl-ex?searchtype=author&query=Aumann%2C+T">T. Aumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">C. Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Holl%2C+M">M. Holl</a>, <a href="/search/nucl-ex?searchtype=author&query=Panin%2C+V">V. Panin</a>, <a href="/search/nucl-ex?searchtype=author&query=Wamers%2C+F">F. Wamers</a>, <a href="/search/nucl-ex?searchtype=author&query=Stroberg%2C+S+R">S. R. Stroberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Holt%2C+J+D">J. D. Holt</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=Alvarez-Pol%2C+H">H. Alvarez-Pol</a>, <a href="/search/nucl-ex?searchtype=author&query=Atar%2C+L">L. Atar</a>, <a href="/search/nucl-ex?searchtype=author&query=Avdeichikov%2C+V">V. Avdeichikov</a>, <a href="/search/nucl-ex?searchtype=author&query=Beceiro-Novo%2C+S">S. Beceiro-Novo</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">J. Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C+A">C. A. Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Bogner%2C+S+K">S. K. Bogner</a>, <a href="/search/nucl-ex?searchtype=author&query=Boillos%2C+J+M">J. M. Boillos</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Borge%2C+M+J+G">M. J. G. Borge</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">E. Casarejos</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W">W. Catford</a> , et al. (85 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="1707.07995v1-abstract-short" style="display: inline;"> Background: Odd-odd nuclei, around doubly closed shells, have been extensively used to study proton-neutron interactions. However, the evolution of these interactions as a function of the binding energy, ultimately when nuclei become unbound, is poorly known. The $^{26}$F nucleus, composed of a deeply bound $\pi0d\_{5/2}$ proton and an unbound $\nu0d\_{3/2}$ neutron on top of an $^{24}$O core, is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.07995v1-abstract-full').style.display = 'inline'; document.getElementById('1707.07995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.07995v1-abstract-full" style="display: none;"> Background: Odd-odd nuclei, around doubly closed shells, have been extensively used to study proton-neutron interactions. However, the evolution of these interactions as a function of the binding energy, ultimately when nuclei become unbound, is poorly known. The $^{26}$F nucleus, composed of a deeply bound $\pi0d\_{5/2}$ proton and an unbound $\nu0d\_{3/2}$ neutron on top of an $^{24}$O core, is particularly adapted for this purpose. The coupling of this proton and neutron results in a $J^蟺 = 1^{+}\_1 - 4^{+}\_1$ multiplet, whose energies must be determined to study the influence of the proximity of the continuum on the corresponding proton-neutron interaction. The $J^蟺 = 1^{+}\_1, 2^{+}\_1,4^{+}\_1$ bound states have been determined, and only a clear identification of the $J^蟺 =3^{+}\_1$ is missing.Purpose: We wish to complete the study of the $J^蟺 = 1^{+}\_1 - 4^{+}\_1$ multiplet in $^{26}$F, by studying the energy and width of the $J^蟺 =3^{+}\_1$ unbound state. The method was firstly validated by the study of unbound states in $^{25}$F, for which resonances were already observed in a previous experiment.Method: Radioactive beams of $^{26}$Ne and $^{27}$Ne, produced at about $440A$\,MeV by the FRagment Separator at the GSI facility, were used to populate unbound states in $^{25}$F and $^{26}$F via one-proton knockout reactions on a CH$\_2$ target, located at the object focal point of the R$^3$B/LAND setup. The detection of emitted $纬$-rays and neutrons, added to the reconstruction of the momentum vector of the $A-1$ nuclei, allowed the determination of the energy of three unbound states in $^{25}$F and two in $^{26}$F. Results: Based on its width and decay properties, the first unbound state in $^{25}$F is proposed to be a $J^蟺 = 1/2^-$ arising from a $p\_{1/2}$ proton-hole state. In $^{26}$F, the first resonance at 323(33)~keV is proposed to be the $J^蟺 =3^{+}\_1$ member of the $J^蟺 = 1^{+}\_1 - 4^{+}\_1$ multiplet. Energies of observed states in $^{25,26}$F have been compared to calculations using the independent-particle shell model, a phenomenological shell-model, and the ab initio valence-space in-medium similarity renormalization group method.Conclusions: The deduced effective proton-neutron interaction is weakened by about 30-40\% in comparison to the models, pointing to the need of implementing the role of the continuum in theoretical descriptions, or to a wrong determination of the atomic mass of $^{26}$F. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.07995v1-abstract-full').style.display = 'none'; document.getElementById('1707.07995v1-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 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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, 7 figures, 3 tables, submitted to 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 96, 054305 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.07952">arXiv:1707.07952</a> <span> [<a href="https://arxiv.org/pdf/1707.07952">pdf</a>, <a href="https://arxiv.org/format/1707.07952">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/10.1016/j.ppnp.2017.09.002">10.1016/j.ppnp.2017.09.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LUNA: Status and Prospects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Trezzi%2C+D">D. Trezzi</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="1707.07952v4-abstract-short" style="display: inline;"> The essential ingredients of nuclear astrophysics are the thermonuclear reactions which shape the life and death of stars and which are responsible for the synthesis of the chemical elements in the Universe. Deep underground in the Gran Sasso Laboratory the cross sections of the key reactions responsible for the hydrogen burning in stars have been measured with two accelerators of 50 and 400 kV vo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.07952v4-abstract-full').style.display = 'inline'; document.getElementById('1707.07952v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.07952v4-abstract-full" style="display: none;"> The essential ingredients of nuclear astrophysics are the thermonuclear reactions which shape the life and death of stars and which are responsible for the synthesis of the chemical elements in the Universe. Deep underground in the Gran Sasso Laboratory the cross sections of the key reactions responsible for the hydrogen burning in stars have been measured with two accelerators of 50 and 400 kV voltage right down to the energies of astrophysical interest. As a matter of fact, the main advantage of the underground laboratory is the reduction of the background. Such a reduction has allowed, for the first time, to measure relevant cross sections at the Gamow energy. The qualifying features of underground nuclear astrophysics are exhaustively reviewed before discussing the current LUNA program which is mainly devoted to the study of the Big-Bang nucleosynthesis and of the synthesis of the light elements in AGB stars and classical novae. The main results obtained during the study of reactions relevant to the Sun are also reviewed and their influence on our understanding of the properties of the neutrino, of the Sun and of the Universe itself is discussed. Finally, the future of LUNA during the next decade is outlined. It will be mainly focused on the study of the nuclear burning stages after hydrogen burning: helium and carbon burning. All this will be accomplished thanks to a new 3.5 MV accelerator able to deliver high current beams of proton, helium and carbon which will start running under Gran Sasso in 2019. In particular, we will discuss the first phase of the scientific case of the 3.5 MV accelerator focused on the study of $^{12}$C+$^{12}$C and of the two reactions which generate free neutrons inside stars: $^{13}$C($伪$,n)$^{16}$O and $^{22}$Ne($伪$,n)$^{25}$Mg. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.07952v4-abstract-full').style.display = 'none'; document.getElementById('1707.07952v4-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> 30 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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">To be published in Progress in Particle and Nuclear Physics 98C (2018) pp. 55-84</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.00925">arXiv:1610.00925</a> <span> [<a href="https://arxiv.org/pdf/1610.00925">pdf</a>, <a href="https://arxiv.org/format/1610.00925">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.94.055804">10.1103/PhysRevC.94.055804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Direct measurement of low-energy $^{22}$Ne(p,$纬$)$^{23}$Na resonances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/nucl-ex?searchtype=author&query=Gy%C3%BCrky%2C+G">Gy. Gy眉rky</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Junker%2C+M">M. Junker</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</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="1610.00925v1-abstract-short" style="display: inline;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction is the most uncertain process in the neon-sodium cycle of hydrogen burning. At temperatures relevant for nucleosynthesis in asymptotic giant branch stars and classical novae, its uncertainty is mainly due to a large number of predicted but hitherto unobserved resonances at low energy. Purpose: A new direct study of low energy $^{22}$Ne(p,$纬$)$^{23}$Na resonan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00925v1-abstract-full').style.display = 'inline'; document.getElementById('1610.00925v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.00925v1-abstract-full" style="display: none;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction is the most uncertain process in the neon-sodium cycle of hydrogen burning. At temperatures relevant for nucleosynthesis in asymptotic giant branch stars and classical novae, its uncertainty is mainly due to a large number of predicted but hitherto unobserved resonances at low energy. Purpose: A new direct study of low energy $^{22}$Ne(p,$纬$)$^{23}$Na resonances has been performed at the Laboratory for Underground Nuclear Astrophysics (LUNA), in the Gran Sasso National Laboratory, Italy. Method: The proton capture on $^{22}$Ne was investigated in direct kinematics, delivering an intense proton beam to a $^{22}$Ne gas target. $纬$ rays were detected with two high-purity germanium detectors enclosed in a copper and lead shielding suppressing environmental radioactivity. Results: Three resonances at 156.2 keV ($蠅纬$ = (1.48\,$\pm$\,0.10)\,$\cdot$\,10$^{-7}$ eV), 189.5 keV ($蠅纬$ = (1.87\,$\pm$\,0.06)\,$\cdot$\,10$^{-6}$ eV) and 259.7 keV ($蠅纬$ = (6.89\,$\pm$\,0.16)\,$\cdot$\,10$^{-6}$ eV) proton beam energy, respectively, have been observed for the first time. For the levels at 8943.5, 8975.3, and 9042.4 keV excitation energy corresponding to the new resonances, the $纬$-decay branching ratios have been precisely measured. Three additional, tentative resonances at 71, 105 and 215 keV proton beam energy, respectively, were not observed here. For the strengths of these resonances, experimental upper limits have been derived that are significantly more stringent than the upper limits reported in the literature. Conclusions: Based on the present experimental data and also previous literature data, an updated thermonuclear reaction rate is provided in tabular and parametric form. The new reaction rate is significantly higher than previous evaluations at temperatures of 0.08-0.3 GK. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00925v1-abstract-full').style.display = 'none'; document.getElementById('1610.00925v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">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 94, 055804 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.00483">arXiv:1610.00483</a> <span> [<a href="https://arxiv.org/pdf/1610.00483">pdf</a>, <a href="https://arxiv.org/format/1610.00483">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.117.142502">10.1103/PhysRevLett.117.142502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved Direct Measurement of the 64.5 keV Resonance Strength in the 17O(p,a)14N Reaction at LUNA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Scott%2C+D+A">D. A. Scott</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fueloep%2C+Z">Zs. Fueloep</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/nucl-ex?searchtype=author&query=Gyurky%2C+G">Gy. Gyurky</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Junker%2C+M">M. Junker</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a> , et al. (10 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="1610.00483v1-abstract-short" style="display: inline;"> The $^{17}$O(p,$伪$)$^{14}$N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as $^{17}$O and $^{18}$F, which can provide constraints on astrophysical models. A new direct determination of the $E_{\rm R}~=~64.5$~keV resonance strength performed at the Laboratory for Underground Nuclear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00483v1-abstract-full').style.display = 'inline'; document.getElementById('1610.00483v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.00483v1-abstract-full" style="display: none;"> The $^{17}$O(p,$伪$)$^{14}$N reaction plays a key role in various astrophysical scenarios, from asymptotic giant branch stars to classical novae. It affects the synthesis of rare isotopes such as $^{17}$O and $^{18}$F, which can provide constraints on astrophysical models. A new direct determination of the $E_{\rm R}~=~64.5$~keV resonance strength performed at the Laboratory for Underground Nuclear Astrophysics accelerator has led to the most accurate value to date, $蠅纬= 10.0 \pm 1.4_{\rm stat} \pm 0.7_{\rm syst}$~neV, thanks to a significant background reduction underground and generally improved experimental conditions. The (bare) proton partial width of the corresponding state at $E_{\rm x} = 5672$~keV in $^{18}$F is $螕_{\rm p} = 35 \pm 5_{\rm stat} \pm 3_{\rm syst}$~neV. This width is about a factor of 2 higher than previously estimated thus leading to a factor of 2 increase in the $^{17}$O(p,$伪$)$^{14}$N reaction rate at astrophysical temperatures relevant to shell hydrogen-burning in red giant and asymptotic giant branch stars. The new rate implies lower $^{17}$O/$^{16}$O ratios, with important implications on the interpretation of astrophysical observables from these stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.00483v1-abstract-full').style.display = 'none'; document.getElementById('1610.00483v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physics Review Letters, 117, 142502 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.05819">arXiv:1609.05819</a> <span> [<a href="https://arxiv.org/pdf/1609.05819">pdf</a>, <a href="https://arxiv.org/format/1609.05819">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/10.7566/JPSCP.14.021106">10.7566/JPSCP.14.021106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Progress of the Felsenkeller shallow-underground accelerator for nuclear astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cowan%2C+T+E">T. E. Cowan</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">T. Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">A. R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">F. Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S+E">S. E. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Rimarzig%2C+B">B. Rimarzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">S. Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Schulz%2C+S">S. Schulz</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1609.05819v1-abstract-short" style="display: inline;"> Low-background experiments with stable ion beams are an important tool for putting the model of stellar hydrogen, helium, and carbon burning on a solid experimental foundation. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso, using a 0.4 MV accelerator. In the present contribution, the status of the project for a higher-energy underground accelerator is rev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05819v1-abstract-full').style.display = 'inline'; document.getElementById('1609.05819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.05819v1-abstract-full" style="display: none;"> Low-background experiments with stable ion beams are an important tool for putting the model of stellar hydrogen, helium, and carbon burning on a solid experimental foundation. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso, using a 0.4 MV accelerator. In the present contribution, the status of the project for a higher-energy underground accelerator is reviewed. Two tunnels of the Felsenkeller underground site in Dresden, Germany, are currently being refurbished for the installation of a 5 MV high-current Pelletron accelerator. Construction work is on schedule and expected to complete in August 2017. The accelerator will provide intense, 50 uA, beams of 1H+, 4He+, and 12C+ ions, enabling research on astrophysically relevant nuclear reactions with unprecedented sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05819v1-abstract-full').style.display = 'none'; document.getElementById('1609.05819v1-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 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Submitted to the Proceedings of Nuclei in the Cosmos XIV, 19-24 June 2016, Niigata/Japan</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.00201">arXiv:1606.00201</a> <span> [<a href="https://arxiv.org/pdf/1606.00201">pdf</a>, <a href="https://arxiv.org/ps/1606.00201">ps</a>, <a href="https://arxiv.org/format/1606.00201">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.93.065807">10.1103/PhysRevC.93.065807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Coulomb dissociation of $^{20,21}$N </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6der%2C+M">Marko R枚der</a>, <a href="/search/nucl-ex?searchtype=author&query=Adachi%2C+T">Tatsuya Adachi</a>, <a href="/search/nucl-ex?searchtype=author&query=Aksyutina%2C+Y">Yulia Aksyutina</a>, <a href="/search/nucl-ex?searchtype=author&query=Alcantara%2C+J">Juan Alcantara</a>, <a href="/search/nucl-ex?searchtype=author&query=Altstadt%2C+S">Sebastian Altstadt</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez-Pol%2C+H">Hector Alvarez-Pol</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashwood%2C+N">Nicholas Ashwood</a>, <a href="/search/nucl-ex?searchtype=author&query=Atar%2C+L">Leyla Atar</a>, <a href="/search/nucl-ex?searchtype=author&query=Aumann%2C+T">Thomas Aumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Avdeichikov%2C+V">Vladimir Avdeichikov</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+M">M. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Beceiro%2C+S">Saul Beceiro</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">Jose Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C">Carlos Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">Konstanze Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Borge%2C+M+J+G">Maria J. G. Borge</a>, <a href="/search/nucl-ex?searchtype=author&query=Burgunder%2C+G">G. Burgunder</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">Manuel Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">Christoph Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">Enrique Casarejos</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W">Wilton Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Cederkall%2C+J">Joakim Cederkall</a>, <a href="/search/nucl-ex?searchtype=author&query=Chakraborty%2C+S">S. Chakraborty</a>, <a href="/search/nucl-ex?searchtype=author&query=Chartier%2C+M">Marielle Chartier</a> , et al. (98 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="1606.00201v1-abstract-short" style="display: inline;"> Neutron-rich light nuclei and their reactions play an important role for the creation of chemical elements. Here, data from a Coulomb dissociation experiment on $^{20,21}$N are reported. Relativistic $^{20,21}$N ions impinged on a lead target and the Coulomb dissociation cross section was determined in a kinematically complete experiment. Using the detailed balance theorem, the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.00201v1-abstract-full').style.display = 'inline'; document.getElementById('1606.00201v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.00201v1-abstract-full" style="display: none;"> Neutron-rich light nuclei and their reactions play an important role for the creation of chemical elements. Here, data from a Coulomb dissociation experiment on $^{20,21}$N are reported. Relativistic $^{20,21}$N ions impinged on a lead target and the Coulomb dissociation cross section was determined in a kinematically complete experiment. Using the detailed balance theorem, the $^{19}\mathrm{N}(\mathrm{n},纬)^{20}\mathrm{N}$ and $^{20}\mathrm{N}(\mathrm{n},纬)^{21}\mathrm{N}$ excitation functions and thermonuclear reaction rates have been determined. The $^{19}\mathrm{N}(\mathrm{n},纬)^{20}\mathrm{N}$ rate is up to a factor of 5 higher at $T<1$\,GK with respect to previous theoretical calculations, leading to a 10\,\% decrease in the predicted fluorine abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.00201v1-abstract-full').style.display = 'none'; document.getElementById('1606.00201v1-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 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 93, 065807 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.02526">arXiv:1605.02526</a> <span> [<a href="https://arxiv.org/pdf/1605.02526">pdf</a>, <a href="https://arxiv.org/ps/1605.02526">ps</a>, <a href="https://arxiv.org/format/1605.02526">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="Materials Science">cond-mat.mtrl-sci</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.nimb.2016.05.009">10.1016/j.nimb.2016.05.009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Absolute hydrogen depth profiling using the resonant $^{1}$H($^{15}$N,$伪纬$)$^{12}$C nuclear reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">Tobias P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=Akhmadaliev%2C+S">Shavkat Akhmadaliev</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">Klaus St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">Louis Wagner</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="1605.02526v1-abstract-short" style="display: inline;"> Resonant nuclear reactions are a powerful tool for the determination of the amount and profile of hydrogen in thin layers of material. Usually, this tool requires the use of a standard of well-known composition. The present work, by contrast, deals with standard-less hydrogen depth profiling. This approach requires precise nuclear data, e.g. on the widely used $^{1}$H($^{15}$N,$伪纬$)$^{12}$C reacti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02526v1-abstract-full').style.display = 'inline'; document.getElementById('1605.02526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.02526v1-abstract-full" style="display: none;"> Resonant nuclear reactions are a powerful tool for the determination of the amount and profile of hydrogen in thin layers of material. Usually, this tool requires the use of a standard of well-known composition. The present work, by contrast, deals with standard-less hydrogen depth profiling. This approach requires precise nuclear data, e.g. on the widely used $^{1}$H($^{15}$N,$伪纬$)$^{12}$C reaction, resonant at 6.4\,MeV $^{15}$N beam energy. Here, the strongly anisotropic angular distribution of the emitted $纬$-rays from this resonance has been re-measured, resolving a previous discrepancy. Coefficients of (0.38$\pm$0.04) and (0.80$\pm$0.04) have been deduced for the second and fourth order Legendre polynomials, respectively. In addition, the resonance strength has been re-evaluated to (25.0$\pm$1.5)\,eV, 10\% higher than previously reported. A simple working formula for the hydrogen concentration is given for cases with known $纬$-ray detection efficiency. Finally, the absolute approach is illustrated using two examples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02526v1-abstract-full').style.display = 'none'; document.getElementById('1605.02526v1-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 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">Journal ref:</span> Nucl. Inst. Meth. B 381, 58-66 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.05832">arXiv:1604.05832</a> <span> [<a href="https://arxiv.org/pdf/1604.05832">pdf</a>, <a href="https://arxiv.org/format/1604.05832">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.95.014613">10.1103/PhysRevC.95.014613 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determination of the Neutron-Capture Rate of 17C for the R-process Nucleosynthesis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Heine%2C+M">M. Heine</a>, <a href="/search/nucl-ex?searchtype=author&query=Typel%2C+S">S. Typel</a>, <a href="/search/nucl-ex?searchtype=author&query=Wu%2C+M+-">M. -R. Wu</a>, <a href="/search/nucl-ex?searchtype=author&query=Adachi%2C+T">T. Adachi</a>, <a href="/search/nucl-ex?searchtype=author&query=Aksyutina%2C+Y">Y. Aksyutina</a>, <a href="/search/nucl-ex?searchtype=author&query=Alcantara%2C+J">J. Alcantara</a>, <a href="/search/nucl-ex?searchtype=author&query=Altstadt%2C+S">S. Altstadt</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=Ashwood%2C+N">N. Ashwood</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>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+M">M. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Beceiro-Novo%2C+S">S. Beceiro-Novo</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">J. Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C+A">C. A. Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Borge%2C+M+J+G">M. J. G. Borge</a>, <a href="/search/nucl-ex?searchtype=author&query=Burgunder%2C+G">G. Burgunder</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">C. Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">E. Casarejos</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W">W. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Cederk%C3%A4ll%2C+J">J. Cederk盲ll</a>, <a href="/search/nucl-ex?searchtype=author&query=Chakraborty%2C+S">S. Chakraborty</a> , et al. (102 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="1604.05832v1-abstract-short" style="display: inline;"> With the R$^{3}$B-LAND setup at GSI we have measured exclusive relative-energy spectra of the Coulomb dissociation of $^{18}$C at a projectile energy around 425~AMeV on a lead target, which are needed to determine the radiative neutron-capture cross sections of $^{17}$C into the ground state of $^{18}$C. Those data have been used to constrain theoretical calculations for transitions populating exc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.05832v1-abstract-full').style.display = 'inline'; document.getElementById('1604.05832v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.05832v1-abstract-full" style="display: none;"> With the R$^{3}$B-LAND setup at GSI we have measured exclusive relative-energy spectra of the Coulomb dissociation of $^{18}$C at a projectile energy around 425~AMeV on a lead target, which are needed to determine the radiative neutron-capture cross sections of $^{17}$C into the ground state of $^{18}$C. Those data have been used to constrain theoretical calculations for transitions populating excited states in $^{18}$C. This allowed to derive the astrophysical cross section $蟽^{*}_{\mathrm{n}纬}$ accounting for the thermal population of $^{17}$C target states in astrophysical scenarios. The experimentally verified capture rate is significantly lower than those of previously obtained Hauser-Feshbach estimations at temperatures $T_{9}\leq{}1$~GK. Network simulations with updated neutron-capture rates and hydrodynamics according to the neutrino-driven wind model as well as the neutron-star merger scenario reveal no pronounced influence of neutron capture of $^{17}$C on the production of second- and third-peak elements in contrast to earlier sensitivity studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.05832v1-abstract-full').style.display = 'none'; document.getElementById('1604.05832v1-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 95, 014613 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1603.00323">arXiv:1603.00323</a> <span> [<a href="https://arxiv.org/pdf/1603.00323">pdf</a>, <a href="https://arxiv.org/format/1603.00323">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.93.054601">10.1103/PhysRevC.93.054601 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Systematic investigation of projectile fragmentation using beams of unstable B and C isotopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Thies%2C+R">R. Thies</a>, <a href="/search/nucl-ex?searchtype=author&query=Heinz%2C+A">A. Heinz</a>, <a href="/search/nucl-ex?searchtype=author&query=Adachi%2C+T">T. Adachi</a>, <a href="/search/nucl-ex?searchtype=author&query=Aksyutina%2C+Y">Y. Aksyutina</a>, <a href="/search/nucl-ex?searchtype=author&query=Alcantara-N%C3%BA%C3%B1es%2C+J">J. Alcantara-N煤帽es</a>, <a href="/search/nucl-ex?searchtype=author&query=Altstadt%2C+S">S. Altstadt</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=Ashwood%2C+N">N. Ashwood</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>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+M">M. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Beceiro-Novo%2C+S">S. Beceiro-Novo</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Benlliure%2C+J">J. Benlliure</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertulani%2C+C+A">C. A. Bertulani</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Borge%2C+M+J+G">M. J. G. Borge</a>, <a href="/search/nucl-ex?searchtype=author&query=Burgunder%2C+G">G. Burgunder</a>, <a href="/search/nucl-ex?searchtype=author&query=Caamano%2C+M">M. Caamano</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">C. Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Casarejos%2C+E">E. Casarejos</a>, <a href="/search/nucl-ex?searchtype=author&query=Catford%2C+W">W. Catford</a>, <a href="/search/nucl-ex?searchtype=author&query=Cederk%C3%A4ll%2C+J">J. Cederk盲ll</a>, <a href="/search/nucl-ex?searchtype=author&query=Chakraborty%2C+S">S. Chakraborty</a>, <a href="/search/nucl-ex?searchtype=author&query=Chartier%2C+M">M. Chartier</a> , et al. (97 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="1603.00323v2-abstract-short" style="display: inline;"> Background: Models describing nuclear fragmentation and fragmentation-fission deliver important input for planning nuclear physics experiments and future radioactive ion beam facilities. These models are usually benchmarked against data from stable beam experiments. In the future, two-step fragmentation reactions with exotic nuclei as stepping stones are a promising tool to reach the most neutron-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00323v2-abstract-full').style.display = 'inline'; document.getElementById('1603.00323v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1603.00323v2-abstract-full" style="display: none;"> Background: Models describing nuclear fragmentation and fragmentation-fission deliver important input for planning nuclear physics experiments and future radioactive ion beam facilities. These models are usually benchmarked against data from stable beam experiments. In the future, two-step fragmentation reactions with exotic nuclei as stepping stones are a promising tool to reach the most neutron-rich nuclei, creating a need for models to describe also these reactions. Purpose: We want to extend the presently available data on fragmentation reactions towards the light exotic region on the nuclear chart. Furthermore, we want to improve the understanding of projectile fragmentation especially for unstable isotopes. Method: We have measured projectile fragments from 10,12-18C and 10-15B isotopes colliding with a carbon target. These measurements were all performed within one experiment, which gives rise to a very consistent dataset. We compare our data to model calculations. Results: One-proton removal cross sections with different final neutron numbers (1pxn) for relativistic 10,12-18C and 10-15B isotopes impinging on a carbon target. Comparing model calculations to the data, we find that EPAX is not able to describe the data satisfactorily. Using ABRABLA07 on the other hand, we find that the average excitation energy per abraded nucleon needs to be decreased from 27 MeV to 8.1 MeV. With that decrease ABRABLA07 describes the data surprisingly well. Conclusions: Extending the available data towards light unstable nuclei with a consistent set of new data have allowed for a systematic investigation of the role of the excitation energy induced in projectile fragmentation. Most striking is the apparent mass dependence of the average excitation energy per abraded nucleon. Nevertheless, this parameter, which has been related to final-state interactions, requires further study. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1603.00323v2-abstract-full').style.display = 'none'; document.getElementById('1603.00323v2-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> 2 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 93, 054601 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.04603">arXiv:1601.04603</a> <span> [<a href="https://arxiv.org/pdf/1601.04603">pdf</a>, <a href="https://arxiv.org/ps/1601.04603">ps</a>, <a href="https://arxiv.org/format/1601.04603">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.2016.01.054">10.1016/j.nima.2016.01.054 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Silicon photomultiplier readout of a monolithic 270$\times$5$\times$5 cm$^3$ plastic scintillator bar for time of flight applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">Tobias P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=Gohl%2C+S">Stefan Gohl</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">Stefan Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cowan%2C+T+E">Thomas E. Cowan</a>, <a href="/search/nucl-ex?searchtype=author&query=Heidel%2C+K">Klaus Heidel</a>, <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6der%2C+M">Marko R枚der</a>, <a href="/search/nucl-ex?searchtype=author&query=Stach%2C+D">Daniel Stach</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">Andreas Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Weinberger%2C+D">David Weinberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="1601.04603v1-abstract-short" style="display: inline;"> The detection of 200-1000 MeV neutrons requires large amounts, $\sim$100 cm, of detector material because of the long nuclear interaction length of these particles. In the example of the NeuLAND neutron time-of-flight detector at FAIR, this is accomplished by using 3000 monolithic scintillator bars of 270$\times$5$\times$5 cm$^3$ size made of a fast plastic. Each bar is read out on the two long en… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.04603v1-abstract-full').style.display = 'inline'; document.getElementById('1601.04603v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.04603v1-abstract-full" style="display: none;"> The detection of 200-1000 MeV neutrons requires large amounts, $\sim$100 cm, of detector material because of the long nuclear interaction length of these particles. In the example of the NeuLAND neutron time-of-flight detector at FAIR, this is accomplished by using 3000 monolithic scintillator bars of 270$\times$5$\times$5 cm$^3$ size made of a fast plastic. Each bar is read out on the two long ends, and the needed time resolution of $蟽_t$ $<$ 150 ps is reached with fast timing photomultipliers. In the present work, it is investigated whether silicon photomultiplier (SiPM) photosensors can be used instead. Experiments with a picosecond laser system were conducted to determine the timing response of the assembly made up of SiPM and preamplifier. The response of the full system including also the scintillator was studied using 30 MeV single electrons provided by the ELBE superconducting electron linac. The ELBE data were matched by a simple Monte Carlo simulation, and they were found to obey an inverse-square-root scaling law. In the electron beam tests, a time resolution of $蟽_t$ = 136 ps was reached with a pure SiPM readout, well within the design parameters for NeuLAND. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.04603v1-abstract-full').style.display = 'none'; document.getElementById('1601.04603v1-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">12 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Inst. Meth. A 816, 16 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.05329">arXiv:1511.05329</a> <span> [<a href="https://arxiv.org/pdf/1511.05329">pdf</a>, <a href="https://arxiv.org/ps/1511.05329">ps</a>, <a href="https://arxiv.org/format/1511.05329">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/PhysRevLett.115.252501">10.1103/PhysRevLett.115.252501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Three new low-energy resonances in the $^{22}$Ne(p,$纬$)$^{23}$Na reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=B%C3%B6ltzig%2C+A">A. B枚ltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=di+Leva%2C+A">A. di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/nucl-ex?searchtype=author&query=Gy%C3%BCrky%2C+G">Gy. Gy眉rky</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Junker%2C+M">M. Junker</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</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="1511.05329v1-abstract-short" style="display: inline;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle affects the synthesis of the elements between $^{20}$Ne and $^{27}$Al in asymptotic giant branch stars and novae. The $^{22}$Ne(p,$纬$)$^{23}$Na reaction rate is very uncertain because of a large number of unobserved resonances lying in the Gamow window. At proton energies below 400\,keV, only… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.05329v1-abstract-full').style.display = 'inline'; document.getElementById('1511.05329v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.05329v1-abstract-full" style="display: none;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle affects the synthesis of the elements between $^{20}$Ne and $^{27}$Al in asymptotic giant branch stars and novae. The $^{22}$Ne(p,$纬$)$^{23}$Na reaction rate is very uncertain because of a large number of unobserved resonances lying in the Gamow window. At proton energies below 400\,keV, only upper limits exist in the literature for the resonance strengths. Previous reaction rate evaluations differ by large factors. In the present work, the first direct observations of the $^{22}$Ne(p,$纬$)$^{23}$Na resonances at 156.2, 189.5, and 259.7\,keV are reported. Their resonance strengths have been derived with 2-7\% uncertainty. In addition, upper limits for three other resonances have been greatly reduced. Data were taken using a windowless $^{22}$Ne gas target and high-purity germanium detectors at the Laboratory for Underground Nuclear Astrophysics in the Gran Sasso laboratory of the National Institute for Nuclear Physics, Italy, taking advantage of the ultra-low background observed deep underground. The new reaction rate is a factor of 5 higher than the recent evaluation at temperatures relevant to novae and asymptotic giant branch stars nucleosynthesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.05329v1-abstract-full').style.display = 'none'; document.getElementById('1511.05329v1-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, 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">6 pages, 4 figures, submitted to Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 115, 252501 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.03893">arXiv:1507.03893</a> <span> [<a href="https://arxiv.org/pdf/1507.03893">pdf</a>, <a href="https://arxiv.org/format/1507.03893">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.92.045807">10.1103/PhysRevC.92.045807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strengths of the resonances at 436, 479, 639, 661, and 1279 keV in the $^{22}$Ne(p,$纬$)$^{23}$Na reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">Rosanna Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">Francesca Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">Federico Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Slemer%2C+A">Alessandra Slemer</a>, <a href="/search/nucl-ex?searchtype=author&query=Al-Abdullah%2C+T">Tariq Al-Abdullah</a>, <a href="/search/nucl-ex?searchtype=author&query=Akhmadaliev%2C+S">Shavkat Akhmadaliev</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">Michael Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Zolt谩n Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Mattei%2C+G">Giovanni Mattei</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">Stefan Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">Konrad Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Scian%2C+C">Carlo Scian</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">Louis Wagner</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="1507.03893v3-abstract-short" style="display: inline;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction is included in the neon-sodium cycle of hydrogen burning. A number of narrow resonances in the Gamow window dominates the thermonuclear reaction rate. Several resonance strengths are only poorly known. As a result, the $^{22}$Ne(p,$纬$)$^{23}$Na thermonuclear reaction rate is the most uncertain rate of the cycle. Here, a new experimental study of the strengths… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.03893v3-abstract-full').style.display = 'inline'; document.getElementById('1507.03893v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.03893v3-abstract-full" style="display: none;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction is included in the neon-sodium cycle of hydrogen burning. A number of narrow resonances in the Gamow window dominates the thermonuclear reaction rate. Several resonance strengths are only poorly known. As a result, the $^{22}$Ne(p,$纬$)$^{23}$Na thermonuclear reaction rate is the most uncertain rate of the cycle. Here, a new experimental study of the strengths of the resonances at 436, 479, 639, 661, and 1279 keV proton beam energy is reported. The data have been obtained using a tantalum target implanted with $^{22}$Ne. The strengths $蠅纬$ of the resonances at 436, 639, and 661 keV have been determined with a relative approach, using the 479 and 1279 keV resonances for normalization. Subsequently, the ratio of resonance strengths of the 479 and 1279 keV resonances was determined, improving the precision of these two standards. The new data are consistent with, but more precise than, the literature with the exception of the resonance at 661 keV, which is found to be less intense by one order of magnitude. In addition, improved branching ratios have been determined for the gamma decay of the resonances at 436, 479, and 639 keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.03893v3-abstract-full').style.display = 'none'; document.getElementById('1507.03893v3-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">Final version, now using the Kelly et al. (2015) data [15] for normalization; 10 pages, 7 figures, 3 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 92, 045807 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.06027">arXiv:1506.06027</a> <span> [<a href="https://arxiv.org/pdf/1506.06027">pdf</a>, <a href="https://arxiv.org/ps/1506.06027">ps</a>, <a href="https://arxiv.org/format/1506.06027">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.92.014315">10.1103/PhysRevC.92.014315 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Determination of gamma-ray widths in $^{15}$N using nuclear resonance fluorescence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Massarczyk%2C+R">R. Massarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Michelagnoli%2C+C">C. Michelagnoli</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">T. P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Ur%2C+C+A">C. A. Ur</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</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="1506.06027v2-abstract-short" style="display: inline;"> The stable nucleus $^{15}$N is the mirror of $^{15}$O, the bottleneck in the hydrogen burning CNO cycle. Most of the $^{15}$N level widths below the proton emission threshold are known from just one nuclear resonance fluorescence (NRF) measurement, with limited precision in some cases. A recent experiment with the AGATA demonstrator array determined level lifetimes using the Doppler Shift Attenuat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.06027v2-abstract-full').style.display = 'inline'; document.getElementById('1506.06027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.06027v2-abstract-full" style="display: none;"> The stable nucleus $^{15}$N is the mirror of $^{15}$O, the bottleneck in the hydrogen burning CNO cycle. Most of the $^{15}$N level widths below the proton emission threshold are known from just one nuclear resonance fluorescence (NRF) measurement, with limited precision in some cases. A recent experiment with the AGATA demonstrator array determined level lifetimes using the Doppler Shift Attenuation Method (DSAM) in $^{15}$O. As a reference and for testing the method, level lifetimes in $^{15}$N have also been determined in the same experiment. The latest compilation of $^{15}$N level properties dates back to 1991. The limited precision in some cases in the compilation calls for a new measurement in order to enable a comparison to the AGATA demonstrator data. The widths of several $^{15}$N levels have been studied with the NRF method. The solid nitrogen compounds enriched in $^{15}$N have been irradiated with bremsstrahlung. The $纬$-rays following the deexcitation of the excited nuclear levels were detected with four HPGe detectors. Integrated photon-scattering cross sections of ten levels below the proton emission threshold have been measured. Partial gamma-ray widths of ground-state transitions were deduced and compared to the literature. The photon scattering cross sections of two levels above the proton emission threshold, but still below other particle emission energies have also been measured, and proton resonance strengths and proton widths were deduced. Gamma and proton widths consistent with the literature values were obtained, but with greatly improved precision. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.06027v2-abstract-full').style.display = 'none'; document.getElementById('1506.06027v2-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> 27 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Final published version, minor grammar changes, 10 pages, 4 figures, 8 tables; An addendum is published where the last section is revised: T. Sz眉cs and P. Mohr, Phys. Rev. C 92, 044328 (2015) [arXiv:1510.04956]</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 92, 014315 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.08171">arXiv:1504.08171</a> <span> [<a href="https://arxiv.org/pdf/1504.08171">pdf</a>, <a href="https://arxiv.org/format/1504.08171">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/10.1088/1748-0221/10/07/P07005">10.1088/1748-0221/10/07/P07005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Response of Multi-strip Multi-gap Resistive Plate Chamber </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Datta%2C+U">Ushasi Datta</a>, <a href="/search/nucl-ex?searchtype=author&query=Chakraborty%2C+S">S. Chakraborty</a>, <a href="/search/nucl-ex?searchtype=author&query=Rahaman%2C+A">A. Rahaman</a>, <a href="/search/nucl-ex?searchtype=author&query=Basu%2C+P">P. Basu</a>, <a href="/search/nucl-ex?searchtype=author&query=Basu%2C+J">J. Basu</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Kempe%2C+M">M. Kempe</a>, <a href="/search/nucl-ex?searchtype=author&query=Munzenberg%2C+G">G. Munzenberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Simon%2C+H">H. Simon</a>, <a href="/search/nucl-ex?searchtype=author&query=Sobiella%2C+M">M. Sobiella</a>, <a href="/search/nucl-ex?searchtype=author&query=Stach%2C+D">D. Stach</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Yakorev%2C+D">D. Yakorev</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="1504.08171v2-abstract-short" style="display: inline;"> A prototype of Multi-strip Multi-gap Resistive Plate chamber (MMRPC) with active area 40 cm $\times$ 20 cm has been developed at SINP, Kolkata. Detailed response of the developed detector was studied with the pulsed electron beam from ELBE at Helmholtz-Zentrum Dresden-Rossendorf. In this report the response of SINP developed MMRPC with different controlling parameters is described in details. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.08171v2-abstract-full').style.display = 'inline'; document.getElementById('1504.08171v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.08171v2-abstract-full" style="display: none;"> A prototype of Multi-strip Multi-gap Resistive Plate chamber (MMRPC) with active area 40 cm $\times$ 20 cm has been developed at SINP, Kolkata. Detailed response of the developed detector was studied with the pulsed electron beam from ELBE at Helmholtz-Zentrum Dresden-Rossendorf. In this report the response of SINP developed MMRPC with different controlling parameters is described in details. The obtained time resolution ($蟽_t$) of the detector after slew correction was 91.5$ \pm $3 ps. Position resolution measured along ($蟽_x$) and across ($蟽_y$) the strip was 2.8$\pm$0.6 cm and 0.58 cm, respectively. The measured absolute efficiency of the detector for minimum ionizing particle like electron was 95.8$\pm$1.3 $\%$. Better timing resolution of the detector can be achieved by restricting the events to a single strip. The response of the detector was mainly in avalanche mode but a few percentage of streamer mode response was also observed. A comparison of the response of these two modes with trigger rate was studied <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.08171v2-abstract-full').style.display = 'none'; document.getElementById('1504.08171v2-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">19 pages, 26 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Instrumentation 10 (2015) 7005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.07394">arXiv:1504.07394</a> <span> [<a href="https://arxiv.org/pdf/1504.07394">pdf</a>, <a href="https://arxiv.org/ps/1504.07394">ps</a>, <a href="https://arxiv.org/format/1504.07394">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"> $纬$ ray spectroscopy of $^{19}$C via single neutron knock-out reaction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Vajta%2C+Z">Zs. Vajta</a>, <a href="/search/nucl-ex?searchtype=author&query=Dombr%C3%A1di%2C+Z">Zs. Dombr谩di</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Aiba%2C+T">T. Aiba</a>, <a href="/search/nucl-ex?searchtype=author&query=Aoi%2C+N">N. Aoi</a>, <a href="/search/nucl-ex?searchtype=author&query=Baba%2C+H">H. Baba</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiss%2C+%C3%81">脕. Kiss</a>, <a href="/search/nucl-ex?searchtype=author&query=Kobayashi%2C+T">T. Kobayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kondo%2C+Y">Y. Kondo</a>, <a href="/search/nucl-ex?searchtype=author&query=Motobayashi%2C+T">T. Motobayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Nakabayashi%2C+T">T. Nakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Nannichi%2C+T">T. Nannichi</a>, <a href="/search/nucl-ex?searchtype=author&query=Sakurai%2C+H">H. Sakurai</a>, <a href="/search/nucl-ex?searchtype=author&query=Sohler%2C+D">D. Sohler</a>, <a href="/search/nucl-ex?searchtype=author&query=Takeuchi%2C+S">S. Takeuchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Tanaka%2C+K">K. Tanaka</a>, <a href="/search/nucl-ex?searchtype=author&query=Togano%2C+Y">Y. Togano</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamada%2C+K">K. Yamada</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+M">M. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Yoneda%2C+K">K. Yoneda</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="1504.07394v1-abstract-short" style="display: inline;"> The one neutron knock-out reaction $^1$H($^{20}$C,$^{19}$C$纬$) was studied at RIKEN using the DALI2 array. A $纬$ ray transition was observed at 198(10) keV. Based on the comparison between the experimental production cross section and theoretical predictions, the transition was assigned to the decay of the 3/2$_1^+$ state to the ground state. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.07394v1-abstract-full" style="display: none;"> The one neutron knock-out reaction $^1$H($^{20}$C,$^{19}$C$纬$) was studied at RIKEN using the DALI2 array. A $纬$ ray transition was observed at 198(10) keV. Based on the comparison between the experimental production cross section and theoretical predictions, the transition was assigned to the decay of the 3/2$_1^+$ state to the ground state. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07394v1-abstract-full').style.display = 'none'; document.getElementById('1504.07394v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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, submitted in Physical Review C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.00457">arXiv:1503.00457</a> <span> [<a href="https://arxiv.org/pdf/1503.00457">pdf</a>, <a href="https://arxiv.org/ps/1503.00457">ps</a>, <a href="https://arxiv.org/format/1503.00457">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/10.1140/epja/i2015-15033-0">10.1140/epja/i2015-15033-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-ray induced background intercomparison with actively shielded HPGe detectors at underground locations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">T. P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Weinberger%2C+D">D. Weinberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1503.00457v2-abstract-short" style="display: inline;"> The main background above 3\,MeV for in-beam nuclear astrophysics studies with $纬$-ray detectors is caused by cosmic-ray induced secondaries. The two commonly used suppression methods, active and passive shielding, against this kind of background were formerly considered only as alternatives in nuclear astrophysics experiments. In this work the study of the effects of active shielding against cosm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.00457v2-abstract-full').style.display = 'inline'; document.getElementById('1503.00457v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.00457v2-abstract-full" style="display: none;"> The main background above 3\,MeV for in-beam nuclear astrophysics studies with $纬$-ray detectors is caused by cosmic-ray induced secondaries. The two commonly used suppression methods, active and passive shielding, against this kind of background were formerly considered only as alternatives in nuclear astrophysics experiments. In this work the study of the effects of active shielding against cosmic-ray induced events at a medium deep location is performed. Background spectra were recorded with two actively shielded HPGe detectors. The experiment was located at 148\,m below the surface of the Earth in the Reiche Zeche mine in Freiberg, Germany. The results are compared to data with the same detectors at the Earth's surface, and at depths of 45\,m and 1400\,m, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.00457v2-abstract-full').style.display = 'none'; document.getElementById('1503.00457v2-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 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Minor errors corrected; final version</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: 33 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1411.2888">arXiv:1411.2888</a> <span> [<a href="https://arxiv.org/pdf/1411.2888">pdf</a>, <a href="https://arxiv.org/ps/1411.2888">ps</a>, <a href="https://arxiv.org/format/1411.2888">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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/i2014-14179-5">10.1140/epja/i2014-14179-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new study of the $^{22}$Ne(p,$纬$)$^{23}$Na reaction deep underground: Feasibility, setup, and first observation of the 186 keV resonance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Menzel%2C+M+-">M. -L. Menzel</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=di+Leva%2C+A">A. di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/nucl-ex?searchtype=author&query=Gy%C3%BCrky%2C+G">Gy. Gy眉rky</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Junker%2C+M">M. Junker</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Prati%2C+P">P. Prati</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez%2C+C+R">C. Rossi Alvarez</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="1411.2888v2-abstract-short" style="display: inline;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle is active in asymptotic giant branch stars as well as in novae and contributes to the nucleosythesis of neon and sodium isotopes. In order to reduce the uncertainties in the predicted nucleosynthesis yields, new experimental efforts to measure the $^{22}$Ne(p,$纬$)$^{23}$Na cross section direc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.2888v2-abstract-full').style.display = 'inline'; document.getElementById('1411.2888v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1411.2888v2-abstract-full" style="display: none;"> The $^{22}$Ne(p,$纬$)$^{23}$Na reaction takes part in the neon-sodium cycle of hydrogen burning. This cycle is active in asymptotic giant branch stars as well as in novae and contributes to the nucleosythesis of neon and sodium isotopes. In order to reduce the uncertainties in the predicted nucleosynthesis yields, new experimental efforts to measure the $^{22}$Ne(p,$纬$)$^{23}$Na cross section directly at the astrophysically relevant energies are needed. In the present work, a feasibility study for a $^{22}$Ne(p,$纬$)$^{23}$Na experiment at the Laboratory for Underground Nuclear Astrophysics (LUNA) 400\,kV accelerator deep underground in the Gran Sasso laboratory, Italy, is reported. The ion beam induced $纬$-ray background has been studied. The feasibility study led to the first observation of the $E_{\rm p}$ = 186\,keV resonance in a direct experiment. An experimental lower limit of 0.12\,$\times$\,10$^{-6}$\,eV has been obtained for the resonance strength. Informed by the feasibility study, a dedicated experimental setup for the $^{22}$Ne(p,$纬$)$^{23}$Na experiment has been developed. The new setup has been characterized by a study of the temperature and pressure profiles. The beam heating effect that reduces the effective neon gas density due to the heating by the incident proton beam has been studied using the resonance scan technique, and the size of this effect has been determined for a neon gas target. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1411.2888v2-abstract-full').style.display = 'none'; document.getElementById('1411.2888v2-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 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 November, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Minor errors corrected; final version</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 (2014) 50: 179 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.5830">arXiv:1406.5830</a> <span> [<a href="https://arxiv.org/pdf/1406.5830">pdf</a>, <a href="https://arxiv.org/ps/1406.5830">ps</a>, <a href="https://arxiv.org/format/1406.5830">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/10.1140/epja/i2014-14112-0">10.1140/epja/i2014-14112-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Efficiency determination of resistive plate chambers for fast quasi-monoenergetic neutrons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6der%2C+M">M. R枚der</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Aumann%2C+T">T. Aumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boretzky%2C+K">K. Boretzky</a>, <a href="/search/nucl-ex?searchtype=author&query=Caesar%2C+C">C. Caesar</a>, <a href="/search/nucl-ex?searchtype=author&query=Cowan%2C+T+E">T. E. Cowan</a>, <a href="/search/nucl-ex?searchtype=author&query=Hehner%2C+J">J. Hehner</a>, <a href="/search/nucl-ex?searchtype=author&query=Heil%2C+M">M. Heil</a>, <a href="/search/nucl-ex?searchtype=author&query=Kempe%2C+M">M. Kempe</a>, <a href="/search/nucl-ex?searchtype=author&query=Maroussov%2C+V">V. Maroussov</a>, <a href="/search/nucl-ex?searchtype=author&query=Nusair%2C+O">O. Nusair</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokofiev%2C+A+V">A. V. Prokofiev</a>, <a href="/search/nucl-ex?searchtype=author&query=Reifarth%2C+R">R. Reifarth</a>, <a href="/search/nucl-ex?searchtype=author&query=Sobiella%2C+M">M. Sobiella</a>, <a href="/search/nucl-ex?searchtype=author&query=Stach%2C+D">D. Stach</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Yakorev%2C+D">D. Yakorev</a>, <a href="/search/nucl-ex?searchtype=author&query=Zilges%2C+A">A. Zilges</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</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="1406.5830v2-abstract-short" style="display: inline;"> Composite detectors made of stainless steel converters and multigap resistive plate chambers have been irradiated with quasi-monoenergetic neutrons with a peak energy of 175MeV. The neutron detection efficiency has been determined using two different methods. The data are in agreement with the output of Monte Carlo simulations. The simulations are then extended to study the response of a hypotheti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.5830v2-abstract-full').style.display = 'inline'; document.getElementById('1406.5830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.5830v2-abstract-full" style="display: none;"> Composite detectors made of stainless steel converters and multigap resistive plate chambers have been irradiated with quasi-monoenergetic neutrons with a peak energy of 175MeV. The neutron detection efficiency has been determined using two different methods. The data are in agreement with the output of Monte Carlo simulations. The simulations are then extended to study the response of a hypothetical array made of these detectors to energetic neutrons from a radioactive ion beam experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.5830v2-abstract-full').style.display = 'none'; document.getElementById('1406.5830v2-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 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Submitted to Eur.Phys.J. A; upgraded version correcting some typos and updating ref. 6</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 (2014) 50: 112 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1404.2062">arXiv:1404.2062</a> <span> [<a href="https://arxiv.org/pdf/1404.2062">pdf</a>, <a href="https://arxiv.org/ps/1404.2062">ps</a>, <a href="https://arxiv.org/format/1404.2062">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.89.045802">10.1103/PhysRevC.89.045802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Strength of the $E_{\text{p}}$=1.842 MeV resonance in the $^{40}$Ca(p,$纬$)$^{41}$Sc reaction revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">Konrad Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Akhmadaliev%2C+S">Shavkat Akhmadaliev</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">Michael Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">Antonio Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Dietz%2C+M">Mirco Dietz</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Zolt谩n Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">Arnd R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Menzel%2C+M">Marie-Luise Menzel</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">Ronald Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">Andreas Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">Kai Zuber</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="1404.2062v1-abstract-short" style="display: inline;"> The strength of the $E_{\rm p} = 1.842$ MeV resonance in the $^{40}$Ca(p,$纬$)$^{41}$Sc reaction is determined with two different methods: First, by an absolute strength measurement using calcium hydroxide targets, and second, relative to the well-determined strength of the resonance triplet at $E_伪$ = 4.5 MeV in the $^{40}$Ca($伪$,$纬$)$^{44}$Ti reaction. The present new value of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.2062v1-abstract-full').style.display = 'inline'; document.getElementById('1404.2062v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1404.2062v1-abstract-full" style="display: none;"> The strength of the $E_{\rm p} = 1.842$ MeV resonance in the $^{40}$Ca(p,$纬$)$^{41}$Sc reaction is determined with two different methods: First, by an absolute strength measurement using calcium hydroxide targets, and second, relative to the well-determined strength of the resonance triplet at $E_伪$ = 4.5 MeV in the $^{40}$Ca($伪$,$纬$)$^{44}$Ti reaction. The present new value of $蠅纬=(0.192\pm0.017)$ eV is 37% (equivalent to $3.5蟽$) higher than the evaluated literature value. In addition, the ratio of the strengths of the 1.842 MeV $^{40}$Ca(p,$纬$)$^{41}$Sc and 4.5 MeV $^{40}$Ca($伪$,$纬$)$^{44}$Ti resonances has been determined to be $0.0229\pm0.0018$. The newly corrected strength of the 1.842-MeV resonance can be used in the future as a normalization point for experiments with calcium targets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1404.2062v1-abstract-full').style.display = 'none'; document.getElementById('1404.2062v1-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">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 89, 045802 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.1974">arXiv:1311.1974</a> <span> [<a href="https://arxiv.org/pdf/1311.1974">pdf</a>, <a href="https://arxiv.org/ps/1311.1974">ps</a>, <a href="https://arxiv.org/format/1311.1974">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.112.072501">10.1103/PhysRevLett.112.072501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nuclear deformation and neutron excess as competing effects for pygmy dipole strength </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Massarczyk%2C+R">R. Massarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=D%C3%B6nau%2C+F">F. D枚nau</a>, <a href="/search/nucl-ex?searchtype=author&query=Frauendorf%2C+S">S. Frauendorf</a>, <a href="/search/nucl-ex?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Beyer%2C+R">R. Beyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhatia%2C+C">C. Bhatia</a>, <a href="/search/nucl-ex?searchtype=author&query=Birgersson%2C+E">E. Birgersson</a>, <a href="/search/nucl-ex?searchtype=author&query=Butterling%2C+M">M. Butterling</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferrari%2C+A">A. Ferrari</a>, <a href="/search/nucl-ex?searchtype=author&query=Gooden%2C+M+E">M. E. Gooden</a>, <a href="/search/nucl-ex?searchtype=author&query=Hannaske%2C+R">R. Hannaske</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">A. R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Kempe%2C+M">M. Kempe</a>, <a href="/search/nucl-ex?searchtype=author&query=Kelley%2C+J+H">J. H. Kelley</a>, <a href="/search/nucl-ex?searchtype=author&query=K%C3%B6gler%2C+T">T. K枚gler</a>, <a href="/search/nucl-ex?searchtype=author&query=Matic%2C+A">A. Matic</a>, <a href="/search/nucl-ex?searchtype=author&query=Menzel%2C+M+L">M. L. Menzel</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S">S. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinhardt%2C+T+P">T. P. Reinhardt</a>, <a href="/search/nucl-ex?searchtype=author&query=R%C3%B6der%2C+M">M. R枚der</a>, <a href="/search/nucl-ex?searchtype=author&query=Rusev%2C+G">G. Rusev</a>, <a href="/search/nucl-ex?searchtype=author&query=Schilling%2C+K+D">K. D. Schilling</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="1311.1974v1-abstract-short" style="display: inline;"> The electromagnetic dipole strength below the neutron-separation energy has been studied for the xenon isotopes with mass numbers A = 124, 128, 132, and 134 in nuclear resonance fluorescence experiments using the ELBE bremsstrahlung facility at Helmholtz-Zentrum Dresden-Rossendorf and the HIgS facility at Triangle Universities Nuclear Laboratory Durham. The systematic study gained new information… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.1974v1-abstract-full').style.display = 'inline'; document.getElementById('1311.1974v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.1974v1-abstract-full" style="display: none;"> The electromagnetic dipole strength below the neutron-separation energy has been studied for the xenon isotopes with mass numbers A = 124, 128, 132, and 134 in nuclear resonance fluorescence experiments using the ELBE bremsstrahlung facility at Helmholtz-Zentrum Dresden-Rossendorf and the HIgS facility at Triangle Universities Nuclear Laboratory Durham. The systematic study gained new information about the influence of the neutron excess as well as of nuclear deformation on the strength in the region of the pygmy dipole resonance. The results are compared with those obtained for the chain of molybdenum isotopes and with predictions of a random-phase approximation in a deformed basis. It turned out that the effect of nuclear deformation plays a minor role compared with the one caused by neutron excess. A global parametrization of the strength in terms of neutron and proton numbers allowed us to derive a formula capable of predicting the summed E1 strengths in the pygmy region for a wide mass range of nuclides. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.1974v1-abstract-full').style.display = 'none'; document.getElementById('1311.1974v1-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 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">5 pages, subimtted to 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/1311.1094">arXiv:1311.1094</a> <span> [<a href="https://arxiv.org/pdf/1311.1094">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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/i2013-13137-1">10.1140/epja/i2013-13137-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutron total cross section measurements of gold and tantalum at the nELBE photoneutron source </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hannaske%2C+R">Roland Hannaske</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Zoltan Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Beyer%2C+R">Roland Beyer</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A">Arnd Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">Daniel Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Birgersson%2C+E">Evert Birgersson</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferrari%2C+A">Anna Ferrari</a>, <a href="/search/nucl-ex?searchtype=author&query=Grosse%2C+E">Eckart Grosse</a>, <a href="/search/nucl-ex?searchtype=author&query=Kempe%2C+M">Mathias Kempe</a>, <a href="/search/nucl-ex?searchtype=author&query=K%C3%B6gler%2C+T">Toni K枚gler</a>, <a href="/search/nucl-ex?searchtype=author&query=Marta%2C+M">Michele Marta</a>, <a href="/search/nucl-ex?searchtype=author&query=Massarczyk%2C+R">Ralph Massarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Matic%2C+A">Andrija Matic</a>, <a href="/search/nucl-ex?searchtype=author&query=Schramm%2C+G">Georg Schramm</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">Ronald Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">Andreas Wagner</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="1311.1094v1-abstract-short" style="display: inline;"> Neutron total cross sections of $^{197}$Au and $^\text{nat}$Ta have been measured at the nELBE photoneutron source in the energy range from 0.1 - 10 MeV with a statistical uncertainty of up to 2 % and a total systematic uncertainty of 1 %. This facility is optimized for the fast neutron energy range and combines an excellent time structure of the neutron pulses (electron bunch width 5 ps) with a s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.1094v1-abstract-full').style.display = 'inline'; document.getElementById('1311.1094v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.1094v1-abstract-full" style="display: none;"> Neutron total cross sections of $^{197}$Au and $^\text{nat}$Ta have been measured at the nELBE photoneutron source in the energy range from 0.1 - 10 MeV with a statistical uncertainty of up to 2 % and a total systematic uncertainty of 1 %. This facility is optimized for the fast neutron energy range and combines an excellent time structure of the neutron pulses (electron bunch width 5 ps) with a short flight path of 7 m. Because of the low instantaneous neutron flux transmission measurements of neutron total cross sections are possible, that exhibit very different beam and background conditions than found at other neutron sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.1094v1-abstract-full').style.display = 'none'; document.getElementById('1311.1094v1-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> 5 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">article (18 pages, 10 figures, 2 tables) with attached data tables (13 pages)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. 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