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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/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/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/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/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/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> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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