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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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/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/2208.12502">arXiv:2208.12502</a> <span> [<a href="https://arxiv.org/pdf/2208.12502">pdf</a>, <a href="https://arxiv.org/format/2208.12502">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/10.3390/universe8010004">10.3390/universe8010004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Underground Measurements of Nuclear Reaction Cross-Sections Relevant to AGB Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ananna%2C+C">Chemseddine Ananna</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">Francesco Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">Axel Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">Carlo Giulio Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">Francesca Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">Giovanni Francesco Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Compagnucci%2C+A">Alessandro Compagnucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">Laszlo Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">Rosanna Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">Federico Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Masha%2C+E">Eliana Masha</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">Denise Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Rapagnani%2C+D">David Rapagnani</a>, <a href="/search/nucl-ex?searchtype=author&query=Skowronski%2C+J">Jakub Skowronski</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="2208.12502v1-abstract-short" style="display: inline;"> Nuclear reaction cross sections are essential ingredients to predict the evolution of AGB stars and understand their impact on the chemical evolution of our Galaxy. Unfortunately, the cross sections of the reactions involved are often very small and challenging to measure in laboratories on Earth. In this context, major steps forward were made with the advent of underground nuclear astrophysics, p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12502v1-abstract-full').style.display = 'inline'; document.getElementById('2208.12502v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.12502v1-abstract-full" style="display: none;"> Nuclear reaction cross sections are essential ingredients to predict the evolution of AGB stars and understand their impact on the chemical evolution of our Galaxy. Unfortunately, the cross sections of the reactions involved are often very small and challenging to measure in laboratories on Earth. In this context, major steps forward were made with the advent of underground nuclear astrophysics, pioneered by the Laboratory for Underground Nuclear Astrophysics (LUNA). The present paper reviews the contribution of LUNA to our understanding of the evolution of AGB stars and related nucleosynthesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12502v1-abstract-full').style.display = 'none'; document.getElementById('2208.12502v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Universe 8(1) (2022) 4 </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/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/1908.07054">arXiv:1908.07054</a> <span> [<a href="https://arxiv.org/pdf/1908.07054">pdf</a>, <a href="https://arxiv.org/format/1908.07054">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/i2019-12859-2">10.1140/epja/i2019-12859-2 <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 $^{10}$B(p,$伪_1 纬$)$^{7}$Be reaction from 0.35 to 1.8 MeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Rigato%2C+V">V. Rigato</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="1908.07054v3-abstract-short" style="display: inline;"> The quantification of isotopes content in materials is extremely important in many research and industrial fields. Accurate determination of boron concentration is very critical in semiconductor, superconductor and steel industry, in environmental and medical applications as well as in nuclear and astrophysics research. The detection of B isotopes and of their ratio in synthetic and natural materi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07054v3-abstract-full').style.display = 'inline'; document.getElementById('1908.07054v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.07054v3-abstract-full" style="display: none;"> The quantification of isotopes content in materials is extremely important in many research and industrial fields. Accurate determination of boron concentration is very critical in semiconductor, superconductor and steel industry, in environmental and medical applications as well as in nuclear and astrophysics research. The detection of B isotopes and of their ratio in synthetic and natural materials may be accomplished by gamma spectroscopy using the $^{10}$B(p,$伪_1 纬$)$^7$Be and $^{11}$B(p,$纬$)$^{12}$C reactions at low proton energy. Here, the $^{10}$B(p,$伪_1 纬$)$^7$Be cross section is reported in the center of mass energy range 0.35 to 1.8 MeV. The $E_纬$= 429 keV $纬$ rays were detected at 45$^\circ$ and 90$^\circ$ using a NaI(Tl) and an HPGe detectors, respectively. In the presented energy range, previous cross sections data revealed discrepancies and normalisation issues. Existing data are compared to the new absolute measurement and discussed. The present data have been subtracted from a previous measurement of the total cross section to derive the contribution of the $伪_0$ channel. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07054v3-abstract-full').style.display = 'none'; document.getElementById('1908.07054v3-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">6 pages, 5 figures</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 (2019) 55: 171 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.05262">arXiv:1902.05262</a> <span> [<a href="https://arxiv.org/pdf/1902.05262">pdf</a>, <a href="https://arxiv.org/format/1902.05262">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="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/10.1393/ncr/i2019-10157-1">10.1393/ncr/i2019-10157-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental nuclear astrophysics in Italy </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=Straniero%2C+O">O. Straniero</a>, <a href="/search/nucl-ex?searchtype=author&query=Taiuti%2C+M+G+F">M. G. F. Taiuti</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Angelis%2C+G">G. de Angelis</a>, <a href="/search/nucl-ex?searchtype=author&query=Benzoni%2C+G">G. Benzoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+G+E">G. E. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Bufalino%2C+S">S. Bufalino</a>, <a href="/search/nucl-ex?searchtype=author&query=Cardella%2C+G">G. Cardella</a>, <a href="/search/nucl-ex?searchtype=author&query=Colonna%2C+N">N. Colonna</a>, <a href="/search/nucl-ex?searchtype=author&query=Contalbrigo%2C+M">M. Contalbrigo</a>, <a href="/search/nucl-ex?searchtype=author&query=Cosentino%2C+G">G. Cosentino</a>, <a href="/search/nucl-ex?searchtype=author&query=Cristallo%2C+S">S. Cristallo</a>, <a href="/search/nucl-ex?searchtype=author&query=Curceanu%2C+C">C. Curceanu</a>, <a href="/search/nucl-ex?searchtype=author&query=De+Filippo%2C+E">E. De Filippo</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=Feliciello%2C+A">A. Feliciello</a>, <a href="/search/nucl-ex?searchtype=author&query=Gammino%2C+S">S. Gammino</a>, <a href="/search/nucl-ex?searchtype=author&query=Galat%C3%A0%2C+A">A. Galat脿</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Lea%2C+R">R. Lea</a>, <a href="/search/nucl-ex?searchtype=author&query=Leoni%2C+S">S. Leoni</a>, <a href="/search/nucl-ex?searchtype=author&query=Lombardo%2C+I">I. Lombardo</a>, <a href="/search/nucl-ex?searchtype=author&query=Manzari%2C+V">V. Manzari</a>, <a href="/search/nucl-ex?searchtype=author&query=Mascali%2C+D">D. Mascali</a> , et al. (14 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="1902.05262v3-abstract-short" style="display: inline;"> Nuclear astrophysics, the union of nuclear physics and astronomy, went through an impressive expansion during the last twenty years. This could be achieved thanks to milestone improvements in astronomical observations, cross section measurements, powerful computer simulations and much refined stellar models. Italian groups are giving quite important contributions to every domain of nuclear astroph… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05262v3-abstract-full').style.display = 'inline'; document.getElementById('1902.05262v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.05262v3-abstract-full" style="display: none;"> Nuclear astrophysics, the union of nuclear physics and astronomy, went through an impressive expansion during the last twenty years. This could be achieved thanks to milestone improvements in astronomical observations, cross section measurements, powerful computer simulations and much refined stellar models. Italian groups are giving quite important contributions to every domain of nuclear astrophysics, sometimes being the leaders of worldwide unique experiments. In this paper we will discuss the astrophysical scenarios where nuclear astrophysics plays a key role and we will provide detailed descriptions of the present and future of the experiments on nuclear astrophysics which belong to the scientific programme of INFN (the National Institute for Nuclear Physics in Italy). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.05262v3-abstract-full').style.display = 'none'; document.getElementById('1902.05262v3-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Added paragraphs 5.6 and 7.2. Paragraph 7.3 (former 7.2) revised. Accepted for publication in La Rivista del Nuovo Cimento</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Rivista del Nuovo Cimento 42, 3 (2019) pp. 103-152 </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/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/1611.06244">arXiv:1611.06244</a> <span> [<a href="https://arxiv.org/pdf/1611.06244">pdf</a>, <a href="https://arxiv.org/format/1611.06244">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/i2016-16075-4">10.1140/epja/i2016-16075-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Shell and explosive hydrogen burning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</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=Cavanna%2C+F">F. Cavanna</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=deBoer%2C+R+J">R. J. deBoer</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=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/nucl-ex?searchtype=author&query=Marigo%2C+P">P. Marigo</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrasi%2C+F">F. Terrasi</a>, <a href="/search/nucl-ex?searchtype=author&query=Wiescher%2C+M">M. Wiescher</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.06244v1-abstract-short" style="display: inline;"> The nucleosynthesis of light elements, from helium up to silicon, mainly occurs in Red Giant and Asymptotic Giant Branch stars and Novae. The relative abundances of the synthesized nuclides critically depend on the rates of the nuclear processes involved, often through non-trivial reaction chains, combined with complex mixing mechanisms. In this review, we summarize the contributions made by LUNA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.06244v1-abstract-full').style.display = 'inline'; document.getElementById('1611.06244v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.06244v1-abstract-full" style="display: none;"> The nucleosynthesis of light elements, from helium up to silicon, mainly occurs in Red Giant and Asymptotic Giant Branch stars and Novae. The relative abundances of the synthesized nuclides critically depend on the rates of the nuclear processes involved, often through non-trivial reaction chains, combined with complex mixing mechanisms. In this review, we summarize the contributions made by LUNA experiments in furthering our understanding of nuclear reaction rates necessary for modeling nucleosynthesis in AGB stars and Novae explosions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.06244v1-abstract-full').style.display = 'none'; document.getElementById('1611.06244v1-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 12 figures</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 (2016) 52: 75 </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/1604.04456">arXiv:1604.04456</a> <span> [<a href="https://arxiv.org/pdf/1604.04456">pdf</a>, <a href="https://arxiv.org/format/1604.04456">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/i2016-16136-8">10.1140/epja/i2016-16136-8 <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 $^{10}$B(p,$伪$)$^{7}$Be reaction at low energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=La+Cognata%2C+M">M. La Cognata</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamia%2C+L">L. Lamia</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Mou%2C+L">L. Mou</a>, <a href="/search/nucl-ex?searchtype=author&query=Puglia%2C+S+M+R">S. M. R. Puglia</a>, <a href="/search/nucl-ex?searchtype=author&query=Rigato%2C+V">V. Rigato</a>, <a href="/search/nucl-ex?searchtype=author&query=Romano%2C+S">S. Romano</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez%2C+C+R">C. Rossi Alvarez</a>, <a href="/search/nucl-ex?searchtype=author&query=Sergi%2C+M+L">M. L. Sergi</a>, <a href="/search/nucl-ex?searchtype=author&query=Spitaleri%2C+C">C. Spitaleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Tumino%2C+A">A. Tumino</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="1604.04456v1-abstract-short" style="display: inline;"> The $^{10}$B(p,$伪$)$^{7}$Be reaction is of great interest since it has many applications in different fields of research such as nuclear astrophysics, nuclear physics, and models of new reactors for clean energy generation. This reaction has been studied at the AN2000 accelerator of the INFN National Laboratories of Legnaro (LNL). The total cross section has been measured in a wide energy range (2… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.04456v1-abstract-full').style.display = 'inline'; document.getElementById('1604.04456v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.04456v1-abstract-full" style="display: none;"> The $^{10}$B(p,$伪$)$^{7}$Be reaction is of great interest since it has many applications in different fields of research such as nuclear astrophysics, nuclear physics, and models of new reactors for clean energy generation. This reaction has been studied at the AN2000 accelerator of the INFN National Laboratories of Legnaro (LNL). The total cross section has been measured in a wide energy range (250 $-$ 1182 keV) by using the activation method. The decays of the $^7$Be nuclei produced by the reaction were measured at the low counting facility of LNL by using two fully shielded high-purity germanium detectors. The present dataset shows a large discrepancy with respect to one of the previous data at the same energies and reduces the total uncertainty to the level of 6\%. An R-matrix calculation has been performed on the present data using the parameters from previous Trojan Horse measurements for the 10 and 500 keV resonances. The present data do not lay on the R-matrix fit in one point suggesting the existence of a $^{11}$C level not observed yet. Further nuclear investigations are needed to confirm this hypothesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.04456v1-abstract-full').style.display = 'none'; document.getElementById('1604.04456v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 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">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to EPJA (6 pages, 3 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/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/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/1409.1362">arXiv:1409.1362</a> <span> [<a href="https://arxiv.org/pdf/1409.1362">pdf</a>, <a href="https://arxiv.org/ps/1409.1362">ps</a>, <a href="https://arxiv.org/format/1409.1362">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/10.1140/epja/i2014-14147-1">10.1140/epja/i2014-14147-1 <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 $^{25}$Mg($伪$,n)$^{28}$Si angular distributions at $E_伪$ = 3 - 5 MeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Marchi%2C+T">T. Marchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Appannababu%2C+S">S. Appannababu</a>, <a href="/search/nucl-ex?searchtype=author&query=Blasi%2C+N">N. Blasi</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Cinausero%2C+M">M. Cinausero</a>, <a href="/search/nucl-ex?searchtype=author&query=Collazuol%2C+G">G. Collazuol</a>, <a href="/search/nucl-ex?searchtype=author&query=Degerlier%2C+M">M. Degerlier</a>, <a href="/search/nucl-ex?searchtype=author&query=Fabris%2C+D">D. Fabris</a>, <a href="/search/nucl-ex?searchtype=author&query=Gramegna%2C+F">F. Gramegna</a>, <a href="/search/nucl-ex?searchtype=author&query=Leone%2C+M">M. Leone</a>, <a href="/search/nucl-ex?searchtype=author&query=Mastinu%2C+P">P. Mastinu</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Montagnoli%2C+G">G. Montagnoli</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez%2C+C+R">C. Rossi Alvarez</a>, <a href="/search/nucl-ex?searchtype=author&query=Rigato%2C+V">V. Rigato</a>, <a href="/search/nucl-ex?searchtype=author&query=Wieland%2C+O">O. Wieland</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="1409.1362v1-abstract-short" style="display: inline;"> The observation of $^{26}$Al gives us the proof of active nucleosynthesis in the Milky Way. However the identification of the main producers of $^{26}$Al is still a matter of debate. Many sites have been proposed, but our poor knowledge of the nuclear processes involved introduces high uncertainties. In particular, the limited accuracy on the $^{25}$Mg($伪$,n)$^{28}$Si reaction cross section has be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1362v1-abstract-full').style.display = 'inline'; document.getElementById('1409.1362v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.1362v1-abstract-full" style="display: none;"> The observation of $^{26}$Al gives us the proof of active nucleosynthesis in the Milky Way. However the identification of the main producers of $^{26}$Al is still a matter of debate. Many sites have been proposed, but our poor knowledge of the nuclear processes involved introduces high uncertainties. In particular, the limited accuracy on the $^{25}$Mg($伪$,n)$^{28}$Si reaction cross section has been identified as the main source of nuclear uncertainty in the production of $^{26}$Al in C/Ne explosive burning in massive stars, which has been suggested to be the main source of $^{26}$Al in the Galaxy. We studied this reaction through neutron spectroscopy at the CN Van de Graaff accelerator of the Legnaro National Laboratories. Thanks to this technique we are able to discriminate the ($伪$,n) events from possible contamination arising from parasitic reactions. In particular, we measured the neutron angular distributions at 5 different beam energies (between 3 and 5 MeV) in the \ang{17.5}-\ang{106} laboratory system angular range. The presented results disagree with the assumptions introduced in the analysis of a previous experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1362v1-abstract-full').style.display = 'none'; document.getElementById('1409.1362v1-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 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">9 pages, 9 figures - accepted by EPJA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1210.0327">arXiv:1210.0327</a> <span> [<a href="https://arxiv.org/pdf/1210.0327">pdf</a>, <a href="https://arxiv.org/format/1210.0327">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/i2012-12144-0">10.1140/epja/i2012-12144-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Preparation and characterisation of isotopically enriched Ta$_2$O$_5$ targets for nuclear astrophysics studies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</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=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</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=Bellini%2C+A">A. Bellini</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=Campeggio%2C+M">M. Campeggio</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</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=Marta%2C+M">M. Marta</a>, <a href="/search/nucl-ex?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/nucl-ex?searchtype=author&query=Napolitani%2C+E">E. Napolitani</a>, <a href="/search/nucl-ex?searchtype=author&query=Prati%2C+P">P. Prati</a>, <a href="/search/nucl-ex?searchtype=author&query=Rigato%2C+V">V. Rigato</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1210.0327v1-abstract-short" style="display: inline;"> The direct measurement of reaction cross sections at astrophysical energies often requires the use of solid targets of known thickness, isotopic composition, and stoichiometry that are able to withstand high beam currents for extended periods of time. Here, we report on the production and characterisation of isotopically enriched Ta$_2$O$_5$ targets for the study of proton-induced reactions at the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.0327v1-abstract-full').style.display = 'inline'; document.getElementById('1210.0327v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1210.0327v1-abstract-full" style="display: none;"> The direct measurement of reaction cross sections at astrophysical energies often requires the use of solid targets of known thickness, isotopic composition, and stoichiometry that are able to withstand high beam currents for extended periods of time. Here, we report on the production and characterisation of isotopically enriched Ta$_2$O$_5$ targets for the study of proton-induced reactions at the Laboratory for Underground Nuclear Astrophysics facility of the Laboratori Nazionali del Gran Sasso. The targets were prepared by anodisation of tantalum backings in enriched water (up to 66% in $^{17}$O and up to 96% in $^{18}$O). Special care was devoted to minimising the presence of any contaminants that could induce unwanted background reactions with the beam in the energy region of astrophysical interest. Results from target characterisation measurements are reported, and the conclusions for proton capture measurements with these targets are drawn. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.0327v1-abstract-full').style.display = 'none'; document.getElementById('1210.0327v1-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, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted to EPJA</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 (2012) 48:144 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.5731">arXiv:1111.5731</a> <span> [<a href="https://arxiv.org/pdf/1111.5731">pdf</a>, <a href="https://arxiv.org/format/1111.5731">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.2011.11.081">10.1016/j.nima.2011.11.081 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> AGATA - Advanced Gamma Tracking Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Akkoyun%2C+S">S. Akkoyun</a>, <a href="/search/nucl-ex?searchtype=author&query=Algora%2C+A">A. Algora</a>, <a href="/search/nucl-ex?searchtype=author&query=Alikhani%2C+B">B. Alikhani</a>, <a href="/search/nucl-ex?searchtype=author&query=Ameil%2C+F">F. Ameil</a>, <a href="/search/nucl-ex?searchtype=author&query=de+Angelis%2C+G">G. de Angelis</a>, <a href="/search/nucl-ex?searchtype=author&query=Arnold%2C+L">L. Arnold</a>, <a href="/search/nucl-ex?searchtype=author&query=Astier%2C+A">A. Astier</a>, <a href="/search/nucl-ex?searchtype=author&query=Ata%C3%A7%2C+A">A. Ata莽</a>, <a href="/search/nucl-ex?searchtype=author&query=Aubert%2C+Y">Y. Aubert</a>, <a href="/search/nucl-ex?searchtype=author&query=Aufranc%2C+C">C. Aufranc</a>, <a href="/search/nucl-ex?searchtype=author&query=Austin%2C+A">A. Austin</a>, <a href="/search/nucl-ex?searchtype=author&query=Aydin%2C+S">S. Aydin</a>, <a href="/search/nucl-ex?searchtype=author&query=Azaiez%2C+F">F. Azaiez</a>, <a href="/search/nucl-ex?searchtype=author&query=Badoer%2C+S">S. Badoer</a>, <a href="/search/nucl-ex?searchtype=author&query=Balabanski%2C+D+L">D. L. Balabanski</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrientos%2C+D">D. Barrientos</a>, <a href="/search/nucl-ex?searchtype=author&query=Baulieu%2C+G">G. Baulieu</a>, <a href="/search/nucl-ex?searchtype=author&query=Baumann%2C+R">R. Baumann</a>, <a href="/search/nucl-ex?searchtype=author&query=Bazzacco%2C+D">D. Bazzacco</a>, <a href="/search/nucl-ex?searchtype=author&query=Beck%2C+F+A">F. A. Beck</a>, <a href="/search/nucl-ex?searchtype=author&query=Beck%2C+T">T. Beck</a>, <a href="/search/nucl-ex?searchtype=author&query=Bednarczyk%2C+P">P. Bednarczyk</a>, <a href="/search/nucl-ex?searchtype=author&query=Bellato%2C+M">M. Bellato</a>, <a href="/search/nucl-ex?searchtype=author&query=Bentley%2C+M+A">M. A. Bentley</a>, <a href="/search/nucl-ex?searchtype=author&query=Benzoni%2C+G">G. Benzoni</a> , et al. (329 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="1111.5731v2-abstract-short" style="display: inline;"> The Advanced GAmma Tracking Array (AGATA) is a European project to develop and operate the next generation gamma-ray spectrometer. AGATA is based on the technique of gamma-ray energy tracking in electrically segmented high-purity germanium crystals. This technique requires the accurate determination of the energy, time and position of every interaction as a gamma ray deposits its energy within the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5731v2-abstract-full').style.display = 'inline'; document.getElementById('1111.5731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.5731v2-abstract-full" style="display: none;"> The Advanced GAmma Tracking Array (AGATA) is a European project to develop and operate the next generation gamma-ray spectrometer. AGATA is based on the technique of gamma-ray energy tracking in electrically segmented high-purity germanium crystals. This technique requires the accurate determination of the energy, time and position of every interaction as a gamma ray deposits its energy within the detector volume. Reconstruction of the full interaction path results in a detector with very high efficiency and excellent spectral response. The realization of gamma-ray tracking and AGATA is a result of many technical advances. These include the development of encapsulated highly-segmented germanium detectors assembled in a triple cluster detector cryostat, an electronics system with fast digital sampling and a data acquisition system to process the data at a high rate. The full characterization of the crystals was measured and compared with detector-response simulations. This enabled pulse-shape analysis algorithms, to extract energy, time and position, to be employed. In addition, tracking algorithms for event reconstruction were developed. The first phase of AGATA is now complete and operational in its first physics campaign. In the future AGATA will be moved between laboratories in Europe and operated in a series of campaigns to take advantage of the different beams and facilities available to maximize its science output. The paper reviews all the achievements made in the AGATA project including all the necessary infrastructure to operate and support the spectrometer. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.5731v2-abstract-full').style.display = 'none'; document.getElementById('1111.5731v2-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 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">This version contains a correction of a typing error in the caption of Fig. 2. The DOI to the article published in Nucl. Instr. 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