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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/2407.10339">arXiv:2407.10339</a> <span> [<a href="https://arxiv.org/pdf/2407.10339">pdf</a>, <a href="https://arxiv.org/format/2407.10339">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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 Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Supernova Pointing Capabilities of DUNE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=DUNE+Collaboration"> DUNE Collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Abud%2C+A+A">A. Abed Abud</a>, <a href="/search/nucl-ex?searchtype=author&query=Abi%2C+B">B. Abi</a>, <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Acero%2C+M+A">M. A. Acero</a>, <a href="/search/nucl-ex?searchtype=author&query=Adames%2C+M+R">M. R. Adames</a>, <a href="/search/nucl-ex?searchtype=author&query=Adamov%2C+G">G. Adamov</a>, <a href="/search/nucl-ex?searchtype=author&query=Adamowski%2C+M">M. Adamowski</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+D">D. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=Adinolfi%2C+M">M. Adinolfi</a>, <a href="/search/nucl-ex?searchtype=author&query=Adriano%2C+C">C. Adriano</a>, <a href="/search/nucl-ex?searchtype=author&query=Aduszkiewicz%2C+A">A. Aduszkiewicz</a>, <a href="/search/nucl-ex?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/nucl-ex?searchtype=author&query=Aimard%2C+B">B. Aimard</a>, <a href="/search/nucl-ex?searchtype=author&query=Akbar%2C+F">F. Akbar</a>, <a href="/search/nucl-ex?searchtype=author&query=Allison%2C+K">K. Allison</a>, <a href="/search/nucl-ex?searchtype=author&query=Monsalve%2C+S+A">S. Alonso Monsalve</a>, <a href="/search/nucl-ex?searchtype=author&query=Alrashed%2C+M">M. Alrashed</a>, <a href="/search/nucl-ex?searchtype=author&query=Alton%2C+A">A. Alton</a>, <a href="/search/nucl-ex?searchtype=author&query=Alvarez%2C+R">R. Alvarez</a>, <a href="/search/nucl-ex?searchtype=author&query=Alves%2C+T">T. Alves</a>, <a href="/search/nucl-ex?searchtype=author&query=Amar%2C+H">H. Amar</a>, <a href="/search/nucl-ex?searchtype=author&query=Amedo%2C+P">P. Amedo</a>, <a href="/search/nucl-ex?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/nucl-ex?searchtype=author&query=Andrade%2C+D+A">D. A. Andrade</a> , et al. (1340 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="2407.10339v1-abstract-short" style="display: inline;"> The determination of the direction of a stellar core collapse via its neutrino emission is crucial for the identification of the progenitor for a multimessenger follow-up. A highly effective method of reconstructing supernova directions within the Deep Underground Neutrino Experiment (DUNE) is introduced. The supernova neutrino pointing resolution is studied by simulating and reconstructing electr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10339v1-abstract-full').style.display = 'inline'; document.getElementById('2407.10339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10339v1-abstract-full" style="display: none;"> The determination of the direction of a stellar core collapse via its neutrino emission is crucial for the identification of the progenitor for a multimessenger follow-up. A highly effective method of reconstructing supernova directions within the Deep Underground Neutrino Experiment (DUNE) is introduced. The supernova neutrino pointing resolution is studied by simulating and reconstructing electron-neutrino charged-current absorption on $^{40}$Ar and elastic scattering of neutrinos on electrons. Procedures to reconstruct individual interactions, including a newly developed technique called ``brems flipping'', as well as the burst direction from an ensemble of interactions are described. Performance of the burst direction reconstruction is evaluated for supernovae happening at a distance of 10 kpc for a specific supernova burst flux model. The pointing resolution is found to be 3.4 degrees at 68% coverage for a perfect interaction-channel classification and a fiducial mass of 40 kton, and 6.6 degrees for a 10 kton fiducial mass respectively. Assuming a 4% rate of charged-current interactions being misidentified as elastic scattering, DUNE's burst pointing resolution is found to be 4.3 degrees (8.7 degrees) at 68% coverage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10339v1-abstract-full').style.display = 'none'; document.getElementById('2407.10339v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">25 pages, 16 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0319-LBNF </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/2310.06082">arXiv:2310.06082</a> <span> [<a href="https://arxiv.org/pdf/2310.06082">pdf</a>, <a href="https://arxiv.org/format/2310.06082">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Measurement of nuclear effects in neutrino-argon interactions using generalized kinematic imbalance variables with the MicroBooNE detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Abratenko%2C+P">P. Abratenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Alterkait%2C+O">O. Alterkait</a>, <a href="/search/nucl-ex?searchtype=author&query=Aldana%2C+D+A">D. Andrade Aldana</a>, <a href="/search/nucl-ex?searchtype=author&query=Arellano%2C+L">L. Arellano</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashkenazi%2C+A">A. Ashkenazi</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrow%2C+D">D. Barrow</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrow%2C+J">J. Barrow</a>, <a href="/search/nucl-ex?searchtype=author&query=Basque%2C+V">V. Basque</a>, <a href="/search/nucl-ex?searchtype=author&query=Rodrigues%2C+O+B">O. Benevides Rodrigues</a>, <a href="/search/nucl-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhanderi%2C+A">A. Bhanderi</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhattacharya%2C+M">M. Bhattacharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bogart%2C+B">B. Bogart</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Book%2C+J+Y">J. Y. Book</a>, <a href="/search/nucl-ex?searchtype=author&query=Brunetti%2C+M+B">M. B. Brunetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a> , et al. (163 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="2310.06082v4-abstract-short" style="display: inline;"> We present a set of new generalized kinematic imbalance variables that can be measured in neutrino scattering. These variables extend previous measurements of kinematic imbalance on the transverse plane, and are more sensitive to modeling of nuclear effects. We demonstrate the enhanced power of these variables using simulation, and then use the MicroBooNE detector to measure them for the first tim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06082v4-abstract-full').style.display = 'inline'; document.getElementById('2310.06082v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06082v4-abstract-full" style="display: none;"> We present a set of new generalized kinematic imbalance variables that can be measured in neutrino scattering. These variables extend previous measurements of kinematic imbalance on the transverse plane, and are more sensitive to modeling of nuclear effects. We demonstrate the enhanced power of these variables using simulation, and then use the MicroBooNE detector to measure them for the first time. We report flux-integrated single- and double-differential measurements of charged-current muon neutrino scattering on argon using a topolgy with one muon and one proton in the final state as a function of these novel kinematic imbalance variables. These measurements allow us to demonstrate that the treatment of charged current quasielastic interactions in GENIE version 2 is inadequate to describe data. Further, they reveal tensions with more modern generator predictions particularly in regions of phase space where final state interactions are important. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06082v4-abstract-full').style.display = 'none'; document.getElementById('2310.06082v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 092007 (2024) </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/2211.03734">arXiv:2211.03734</a> <span> [<a href="https://arxiv.org/pdf/2211.03734">pdf</a>, <a href="https://arxiv.org/format/2211.03734">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> First Measurement of Differential Cross Sections for Muon Neutrino Charged Current Interactions on Argon with a Two-proton Final State in the MicroBooNE Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Abratenko%2C+P">P. Abratenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Aldana%2C+D+A">D. Andrade Aldana</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Arellano%2C+L">L. Arellano</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashkenazi%2C+A">A. Ashkenazi</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Barrow%2C+J">J. Barrow</a>, <a href="/search/nucl-ex?searchtype=author&query=Basque%2C+V">V. Basque</a>, <a href="/search/nucl-ex?searchtype=author&query=Bathe-Peters%2C+L">L. Bathe-Peters</a>, <a href="/search/nucl-ex?searchtype=author&query=Rodrigues%2C+O+B">O. Benevides Rodrigues</a>, <a href="/search/nucl-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhanderi%2C+A">A. Bhanderi</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhattacharya%2C+M">M. Bhattacharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bogart%2C+B">B. Bogart</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Book%2C+J+Y">J. Y. Book</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrazas%2C+I+C">I. Caro Terrazas</a> , et al. (161 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="2211.03734v2-abstract-short" style="display: inline;"> We present the first measurement of differential cross sections for charged-current muon neutrino interactions on argon with one muon, two protons, and no pions in the final state. Such interactions leave the target nucleus in a two-particle two-hole state; these states are of great interest, but currently there is limited information about their production in neutrino-nucleus interactions. Detail… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03734v2-abstract-full').style.display = 'inline'; document.getElementById('2211.03734v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03734v2-abstract-full" style="display: none;"> We present the first measurement of differential cross sections for charged-current muon neutrino interactions on argon with one muon, two protons, and no pions in the final state. Such interactions leave the target nucleus in a two-particle two-hole state; these states are of great interest, but currently there is limited information about their production in neutrino-nucleus interactions. Detailed investigations of the production of two-particle two-hole states are vital to support upcoming experiments exploring the nature of the neutrino, and the development of the liquid-argon time-projection-chamber has made possible the isolation of such final states. The opening angle between the two protons, the angle between the total proton momentum and the muon, and the total transverse momentum of the final state system are sensitive to the underlying physics processes as embodied in a variety of models. Realistic initial-state momentum distributions are shown to be important in reproducing the data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03734v2-abstract-full').style.display = 'none'; document.getElementById('2211.03734v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Resubmitted to PRL in response to reviewer comments</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-836-ND </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/2208.09283">arXiv:2208.09283</a> <span> [<a href="https://arxiv.org/pdf/2208.09283">pdf</a>, <a href="https://arxiv.org/format/2208.09283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3389/fspas.2020.617946">10.3389/fspas.2020.617946 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The study of key reactions shaping the post main-sequence evolution of massive stars in underground facilities </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=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Zavatarelli%2C+S">S. Zavatarelli</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="2208.09283v1-abstract-short" style="display: inline;"> The chemical evolution of the Universe and several phases of the stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross sections at the energies at which they take place in stellar environments. Direct cross-section measurements are mainly hampered by the very low counting rate and by cosmic background, nevertheless they have become… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09283v1-abstract-full').style.display = 'inline'; document.getElementById('2208.09283v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.09283v1-abstract-full" style="display: none;"> The chemical evolution of the Universe and several phases of the stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross sections at the energies at which they take place in stellar environments. Direct cross-section measurements are mainly hampered by the very low counting rate and by cosmic background, nevertheless they have become possible by combining the best experimental techniques with the cosmic silence of an underground laboratory. In the nineties the LUNA (Laboratory for Underground Nuclear Astrophysics) collaboration opened the era of underground nuclear astrophysics installing first a home-made 50 kV and later on, a second 400 kV accelerator under the Gran Sasso mountain in Italy: in 25 years of experimental activity, important reactions responsible for hydrogen burning could have been studied down to the relevant energies thanks to the high current proton and helium beams provided by the machines. The interest to the next and warmer stages of star evolution (i.e. post main sequence, helium and carbon burning) drove a new project based on an ion accelerator in the MV range called LUNA-MV, able to deliver proton, helium and carbon beams. The present contribution is aimed to discuss the state-of-the-art for some selected key processes of post main sequence stellar phases: the 12Cag and the 12C+12C fundamental for helium and carbon burning phases, and 13Can and 22Neag that are relevant to the synthesis of heavy elements in AGB stars. The perspectives opened by an underground MV-facility will be highlighted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.09283v1-abstract-full').style.display = 'none'; document.getElementById('2208.09283v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Front. Astron. Space Sci. 7:617946 (2021) </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/2010.02390">arXiv:2010.02390</a> <span> [<a href="https://arxiv.org/pdf/2010.02390">pdf</a>, <a href="https://arxiv.org/format/2010.02390">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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/10.1103/PhysRevD.102.112013">10.1103/PhysRevD.102.112013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of Differential Cross Sections for $谓_渭$-Ar Charged-Current Interactions with Protons and no Pions in the Final State with the MicroBooNE Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Abratenko%2C+P">P. Abratenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Alrashed%2C+M">M. Alrashed</a>, <a href="/search/nucl-ex?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashkenazi%2C+A">A. Ashkenazi</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnes%2C+C">C. Barnes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Basque%2C+V">V. Basque</a>, <a href="/search/nucl-ex?searchtype=author&query=Bathe-Peters%2C+L">L. Bathe-Peters</a>, <a href="/search/nucl-ex?searchtype=author&query=Rodrigues%2C+O+B">O. Benevides Rodrigues</a>, <a href="/search/nucl-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhanderi%2C+A">A. Bhanderi</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrazas%2C+I+C">I. Caro Terrazas</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+R+C">R. Castillo Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a> , et al. (160 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="2010.02390v1-abstract-short" style="display: inline;"> We present an analysis of MicroBooNE data with a signature of one muon, no pions, and at least one proton above a momentum threshold of 300 MeV/c (CC0$蟺$Np). This is the first differential cross section measurement of this topology in neutrino-argon interactions. We achieve a significantly lower proton momentum threshold than previous carbon and scintillator-based experiments. Using data collected… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02390v1-abstract-full').style.display = 'inline'; document.getElementById('2010.02390v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.02390v1-abstract-full" style="display: none;"> We present an analysis of MicroBooNE data with a signature of one muon, no pions, and at least one proton above a momentum threshold of 300 MeV/c (CC0$蟺$Np). This is the first differential cross section measurement of this topology in neutrino-argon interactions. We achieve a significantly lower proton momentum threshold than previous carbon and scintillator-based experiments. Using data collected from a total of approximately $1.6 \times 10^{20}$ protons-on-target, we measure the muon neutrino cross section for the CC0$蟺$Np interaction channel in argon at MicroBooNE in the Booster Neutrino Beam which has a mean energy of around 800 MeV. We present the results from a data sample with estimated efficiency of 29\% and purity of 76\% as differential cross sections in five reconstructed variables: the muon momentum and polar angle, the leading proton momentum and polar angle, and the muon-proton opening angle. We include smearing matrices that can be used to "forward-fold" theoretical predictions for comparison with these data. We compare the measured differential cross sections to a number of recent theory predictions demonstrating largely good agreement with this first-ever data set on argon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.02390v1-abstract-full').style.display = 'none'; document.getElementById('2010.02390v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">24 pages, 43 figures, 1 table and supplemental material</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-505-AD-ND-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 112013 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.06647">arXiv:2008.06647</a> <span> [<a href="https://arxiv.org/pdf/2008.06647">pdf</a>, <a href="https://arxiv.org/format/2008.06647">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <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/epjc/s10052-021-09166-w">10.1140/epjc/s10052-021-09166-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Supernova Neutrino Burst Detection with the Deep Underground Neutrino Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=DUNE+collaboration"> DUNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Abi%2C+B">B. Abi</a>, <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Acero%2C+M+A">M. A. Acero</a>, <a href="/search/nucl-ex?searchtype=author&query=Adamov%2C+G">G. Adamov</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+D">D. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=Adinolfi%2C+M">M. Adinolfi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ahmad%2C+Z">Z. Ahmad</a>, <a href="/search/nucl-ex?searchtype=author&query=Ahmed%2C+J">J. Ahmed</a>, <a href="/search/nucl-ex?searchtype=author&query=Alion%2C+T">T. Alion</a>, <a href="/search/nucl-ex?searchtype=author&query=Monsalve%2C+S+A">S. Alonso Monsalve</a>, <a href="/search/nucl-ex?searchtype=author&query=Alt%2C+C">C. Alt</a>, <a href="/search/nucl-ex?searchtype=author&query=Anderson%2C+J">J. Anderson</a>, <a href="/search/nucl-ex?searchtype=author&query=Andreopoulos%2C+C">C. Andreopoulos</a>, <a href="/search/nucl-ex?searchtype=author&query=Andrews%2C+M+P">M. P. Andrews</a>, <a href="/search/nucl-ex?searchtype=author&query=Andrianala%2C+F">F. Andrianala</a>, <a href="/search/nucl-ex?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/nucl-ex?searchtype=author&query=Ankowski%2C+A">A. Ankowski</a>, <a href="/search/nucl-ex?searchtype=author&query=Antonova%2C+M">M. Antonova</a>, <a href="/search/nucl-ex?searchtype=author&query=Antusch%2C+S">S. Antusch</a>, <a href="/search/nucl-ex?searchtype=author&query=Aranda-Fernandez%2C+A">A. Aranda-Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Ariga%2C+A">A. Ariga</a>, <a href="/search/nucl-ex?searchtype=author&query=Arnold%2C+L+O">L. O. Arnold</a>, <a href="/search/nucl-ex?searchtype=author&query=Arroyave%2C+M+A">M. A. Arroyave</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a> , et al. (949 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="2008.06647v3-abstract-short" style="display: inline;"> The Deep Underground Neutrino Experiment (DUNE), a 40-kton underground liquid argon time projection chamber experiment, will be sensitive to the electron-neutrino flavor component of the burst of neutrinos expected from the next Galactic core-collapse supernova. Such an observation will bring unique insight into the astrophysics of core collapse as well as into the properties of neutrinos. The gen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06647v3-abstract-full').style.display = 'inline'; document.getElementById('2008.06647v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.06647v3-abstract-full" style="display: none;"> The Deep Underground Neutrino Experiment (DUNE), a 40-kton underground liquid argon time projection chamber experiment, will be sensitive to the electron-neutrino flavor component of the burst of neutrinos expected from the next Galactic core-collapse supernova. Such an observation will bring unique insight into the astrophysics of core collapse as well as into the properties of neutrinos. The general capabilities of DUNE for neutrino detection in the relevant few- to few-tens-of-MeV neutrino energy range will be described. As an example, DUNE's ability to constrain the $谓_e$ spectral parameters of the neutrino burst will be considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06647v3-abstract-full').style.display = 'none'; document.getElementById('2008.06647v3-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">29 pages, 17 figures; paper based on DUNE Technical Design Report. arXiv admin note: substantial text overlap with arXiv:2002.03005</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-380-LBNF </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.00108">arXiv:2006.00108</a> <span> [<a href="https://arxiv.org/pdf/2006.00108">pdf</a>, <a href="https://arxiv.org/format/2006.00108">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.125.201803">10.1103/PhysRevLett.125.201803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Measurement of Differential Charged Current Quasielastic-like $谓_渭$-Argon Scattering Cross Sections with the MicroBooNE Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Abratenko%2C+P">P. Abratenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Alrashed%2C+M">M. Alrashed</a>, <a href="/search/nucl-ex?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashkenazi%2C+A">A. Ashkenazi</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnes%2C+C">C. Barnes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Basque%2C+V">V. Basque</a>, <a href="/search/nucl-ex?searchtype=author&query=Bathe-Peters%2C+L">L. Bathe-Peters</a>, <a href="/search/nucl-ex?searchtype=author&query=Rodrigues%2C+O+B">O. Benevides Rodrigues</a>, <a href="/search/nucl-ex?searchtype=author&query=Berkman%2C+S">S. Berkman</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhanderi%2C+A">A. Bhanderi</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrazas%2C+I+C">I. Caro Terrazas</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+R+C">R. Castillo Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cerati%2C+G">G. Cerati</a> , et al. (159 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="2006.00108v3-abstract-short" style="display: inline;"> We report on the first measurement of flux-integrated single differential cross sections for charged-current (CC) muon neutrino ($谓_渭$) scattering on argon with a muon and a proton in the final state, $^{40}$Ar($谓_渭$,$渭$p)X. The measurement was carried out using the Booster Neutrino Beam at Fermi National Accelerator Laboratory and the MicroBooNE liquid argon time projection chamber detector with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.00108v3-abstract-full').style.display = 'inline'; document.getElementById('2006.00108v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.00108v3-abstract-full" style="display: none;"> We report on the first measurement of flux-integrated single differential cross sections for charged-current (CC) muon neutrino ($谓_渭$) scattering on argon with a muon and a proton in the final state, $^{40}$Ar($谓_渭$,$渭$p)X. The measurement was carried out using the Booster Neutrino Beam at Fermi National Accelerator Laboratory and the MicroBooNE liquid argon time projection chamber detector with an exposure of 4.59 $\times$ 10$^{19}$ protons on target. Events are selected to enhance the contribution of CC quasielastic (CCQE) interactions. The data are reported in terms of a total cross section as well as single differential cross sections in final state muon and proton kinematics. We measure the integrated per-nucleus CCQE-like cross section (i.e. for interactions leading to a muon, one proton and no pions above detection threshold) of (4.93 $\pm$ 0.76stat $\pm$ 1.29sys) $\times$ 10$^{-38}$cm$^2$, in good agreement with theoretical calculations. The single differential cross sections are also in overall good agreement with theoretical predictions, except at very forward muon scattering angles that correspond to low momentum-transfer events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.00108v3-abstract-full').style.display = 'none'; document.getElementById('2006.00108v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in PRL. 8 pages, 3 figures, 1 table and online supplementary materials</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FNAL PUB-20-226-ND </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 125, 201803 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2005.00002">arXiv:2005.00002</a> <span> [<a href="https://arxiv.org/pdf/2005.00002">pdf</a>, <a href="https://arxiv.org/format/2005.00002">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-020-00149-1">10.1140/epja/s10050-020-00149-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Setup commissioning for an improved measurement of the D(p,gamma)3He cross section at Big Bang Nucleosynthesis energies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/nucl-ex?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a> , et al. (22 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2005.00002v1-abstract-short" style="display: inline;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3H… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'inline'; document.getElementById('2005.00002v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.00002v1-abstract-full" style="display: none;"> Among the reactions involved in the production and destruction of deuterium during Big Bang Nucleosynthesis, the deuterium-burning D(p,gamma)3He reaction has the largest uncertainty and limits the precision of theoretical estimates of primordial deuterium abundance. Here we report the results of a careful commissioning of the experimental setup used to measure the cross-section of the D(p,gamma)3He reaction at the Laboratory for Underground Nuclear Astrophysics of the Gran Sasso Laboratory (Italy). The commissioning was aimed at minimising all sources of systematic uncertainty in the measured cross sections. The overall systematic error achieved (< 3 %) will enable improved predictions of BBN deuterium abundance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.00002v1-abstract-full').style.display = 'none'; document.getElementById('2005.00002v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2001.08744">arXiv:2001.08744</a> <span> [<a href="https://arxiv.org/pdf/2001.08744">pdf</a>, <a href="https://arxiv.org/ps/2001.08744">ps</a>, <a href="https://arxiv.org/format/2001.08744">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/s10050-020-00077-0">10.1140/epja/s10050-020-00077-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new approach to monitor 13C-targets degradation in situ for 13C(alpha,n)16O cross-section measurements at LUNA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Paolo%2C+L">L. Di Paolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2001.08744v2-abstract-short" style="display: inline;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section resu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'inline'; document.getElementById('2001.08744v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2001.08744v2-abstract-full" style="display: none;"> Direct measurements of reaction cross-sections at astrophysical energies often require the use of solid targets able to withstand high ion beam currents for extended periods of time. Thus, monitoring target thickness, isotopic composition, and target stoichiometry during data taking is critical to account for possible target modifications and to reduce uncertainties in the final cross-section results. A common technique used for these purposes is the Nuclear Resonant Reaction Analysis (NRRA), which however requires that a narrow resonance be available inside the dynamic range of the accelerator used. In cases when this is not possible, as for example the 13C(alpha,n)16O reaction recently studied at low energies at the Laboratory for Underground Nuclear Astrophysics (LUNA) in Italy, alternative approaches must be found. Here, we present a new application of the shape analysis of primary gamma rays emitted by the 13C(p,g)14N radiative capture reaction. This approach was used to monitor 13C target degradation {\em in situ} during the 13C(alpha,n)16O data taking campaign. The results obtained are in agreement with evaluations subsequently performed at Atomki (Hungary) using the NRRA method. A preliminary application for the extraction of the 13C(alpha,n)16O reaction cross-section at one beam energy is also reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2001.08744v2-abstract-full').style.display = 'none'; document.getElementById('2001.08744v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 6 figures, to be published in EPJ A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The European Physical Journal A volume 56, Article number: 75 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.05679">arXiv:1812.05679</a> <span> [<a href="https://arxiv.org/pdf/1812.05679">pdf</a>, <a href="https://arxiv.org/format/1812.05679">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Rejecting cosmic background for exclusive neutrino interaction studies with Liquid Argon TPCs; a case study with the MicroBooNE detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=Alrashed%2C+M">M. Alrashed</a>, <a href="/search/nucl-ex?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Ashkenazi%2C+A">A. Ashkenazi</a>, <a href="/search/nucl-ex?searchtype=author&query=Auger%2C+M">M. Auger</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnes%2C+C">C. Barnes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Bass%2C+M">M. Bass</a>, <a href="/search/nucl-ex?searchtype=author&query=Bay%2C+F">F. Bay</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhattacharya%2C+K">K. Bhattacharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrazas%2C+I+C">I. Caro Terrazas</a>, <a href="/search/nucl-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+R+C">R. Castillo Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a> , et al. (150 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="1812.05679v2-abstract-short" style="display: inline;"> Cosmic ray (CR) interactions can be a challenging source of background for neutrino oscillation and cross-section measurements in surface detectors. We present methods for CR rejection in measurements of charged-current quasielastic-like (CCQE-like) neutrino interactions, with a muon and a proton in the final state, measured using liquid argon time projection chambers (LArTPCs). Using a sample of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05679v2-abstract-full').style.display = 'inline'; document.getElementById('1812.05679v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.05679v2-abstract-full" style="display: none;"> Cosmic ray (CR) interactions can be a challenging source of background for neutrino oscillation and cross-section measurements in surface detectors. We present methods for CR rejection in measurements of charged-current quasielastic-like (CCQE-like) neutrino interactions, with a muon and a proton in the final state, measured using liquid argon time projection chambers (LArTPCs). Using a sample of cosmic data collected with the MicroBooNE detector, mixed with simulated neutrino scattering events, a set of event selection criteria is developed that produces an event sample with minimal contribution from CR background. Depending on the selection criteria used a purity between 50% and 80% can be achieved with a signal selection efficiency between 50% and 25%, with higher purity coming at the expense of lower efficiency. While using a specific dataset from the MicroBooNE detector and selection criteria values optimized for CCQE-like events, the concepts presented here are generic and can be adapted for various studies of exclusive 谓渭 interactions in LArTPCs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.05679v2-abstract-full').style.display = 'none'; document.getElementById('1812.05679v2-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-18-677-E </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/1804.02583">arXiv:1804.02583</a> <span> [<a href="https://arxiv.org/pdf/1804.02583">pdf</a>, <a href="https://arxiv.org/format/1804.02583">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/13/07/P07007">10.1088/1748-0221/13/07/P07007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionization Electron Signal Processing in Single Phase LArTPCs II. Data/Simulation Comparison and Performance in MicroBooNE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Auger%2C+M">M. Auger</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnes%2C+C">C. Barnes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Bass%2C+M">M. Bass</a>, <a href="/search/nucl-ex?searchtype=author&query=Bay%2C+F">F. Bay</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhattacharya%2C+K">K. Bhattacharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Carr%2C+R">R. Carr</a>, <a href="/search/nucl-ex?searchtype=author&query=Terrazas%2C+I+C">I. Caro Terrazas</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+R+C">R. Castillo Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cerati%2C+G">G. Cerati</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+H">H. Chen</a> , et al. (146 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="1804.02583v3-abstract-short" style="display: inline;"> The single-phase liquid argon time projection chamber (LArTPC) provides a large amount of detailed information in the form of fine-grained drifted ionization charge from particle traces. To fully utilize this information, the deposited charge must be accurately extracted from the raw digitized waveforms via a robust signal processing chain. Enabled by the ultra-low noise levels associated with cry… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.02583v3-abstract-full').style.display = 'inline'; document.getElementById('1804.02583v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.02583v3-abstract-full" style="display: none;"> The single-phase liquid argon time projection chamber (LArTPC) provides a large amount of detailed information in the form of fine-grained drifted ionization charge from particle traces. To fully utilize this information, the deposited charge must be accurately extracted from the raw digitized waveforms via a robust signal processing chain. Enabled by the ultra-low noise levels associated with cryogenic electronics in the MicroBooNE detector, the precise extraction of ionization charge from the induction wire planes in a single-phase LArTPC is qualitatively demonstrated on MicroBooNE data with event display images, and quantitatively demonstrated via waveform-level and track-level metrics. Improved performance of induction plane calorimetry is demonstrated through the agreement of extracted ionization charge measurements across different wire planes for various event topologies. In addition to the comprehensive waveform-level comparison of data and simulation, a calibration of the cryogenic electronics response is presented and solutions to various MicroBooNE-specific TPC issues are discussed. This work presents an important improvement in LArTPC signal processing, the foundation of reconstruction and therefore physics analyses in MicroBooNE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.02583v3-abstract-full').style.display = 'none'; document.getElementById('1804.02583v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">54 pages, 36 figures; the first part of this work can be found at arXiv:1802.08709</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 13 P07007 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.08709">arXiv:1802.08709</a> <span> [<a href="https://arxiv.org/pdf/1802.08709">pdf</a>, <a href="https://arxiv.org/format/1802.08709">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/13/07/P07006">10.1088/1748-0221/13/07/P07006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionization Electron Signal Processing in Single Phase LArTPCs I. Algorithm Description and Quantitative Evaluation with MicroBooNE Simulation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=MicroBooNE+collaboration"> MicroBooNE collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/nucl-ex?searchtype=author&query=Anthony%2C+J">J. Anthony</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Auger%2C+M">M. Auger</a>, <a href="/search/nucl-ex?searchtype=author&query=Bagby%2C+L">L. Bagby</a>, <a href="/search/nucl-ex?searchtype=author&query=Balasubramanian%2C+S">S. Balasubramanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Barnes%2C+C">C. Barnes</a>, <a href="/search/nucl-ex?searchtype=author&query=Barr%2C+G">G. Barr</a>, <a href="/search/nucl-ex?searchtype=author&query=Bass%2C+M">M. Bass</a>, <a href="/search/nucl-ex?searchtype=author&query=Bay%2C+F">F. Bay</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhat%2C+A">A. Bhat</a>, <a href="/search/nucl-ex?searchtype=author&query=Bhattacharya%2C+K">K. Bhattacharya</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/nucl-ex?searchtype=author&query=Blake%2C+A">A. Blake</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Camilleri%2C+L">L. Camilleri</a>, <a href="/search/nucl-ex?searchtype=author&query=Caratelli%2C+D">D. Caratelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez%2C+R+C">R. Castillo Fernandez</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cerati%2C+G">G. Cerati</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+H">H. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+Y">Y. Chen</a> , et al. (144 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="1802.08709v3-abstract-short" style="display: inline;"> We describe the concept and procedure of drifted-charge extraction developed in the MicroBooNE experiment, a single-phase liquid argon time projection chamber (LArTPC). This technique converts the raw digitized TPC waveform to the number of ionization electrons passing through a wire plane at a given time. A robust recovery of the number of ionization electrons from both induction and collection a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08709v3-abstract-full').style.display = 'inline'; document.getElementById('1802.08709v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.08709v3-abstract-full" style="display: none;"> We describe the concept and procedure of drifted-charge extraction developed in the MicroBooNE experiment, a single-phase liquid argon time projection chamber (LArTPC). This technique converts the raw digitized TPC waveform to the number of ionization electrons passing through a wire plane at a given time. A robust recovery of the number of ionization electrons from both induction and collection anode wire planes will augment the 3D reconstruction, and is particularly important for tomographic reconstruction algorithms. A number of building blocks of the overall procedure are described. The performance of the signal processing is quantitatively evaluated by comparing extracted charge with the true charge through a detailed TPC detector simulation taking into account position-dependent induced current inside a single wire region and across multiple wires. Some areas for further improvement of the performance of the charge extraction procedure are also discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.08709v3-abstract-full').style.display = 'none'; document.getElementById('1802.08709v3-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">60 pages, 36 figures. The second part of this work can be found at arXiv:1804.02583</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 13 P07006 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1802.04164">arXiv:1802.04164</a> <span> [<a href="https://arxiv.org/pdf/1802.04164">pdf</a>, <a href="https://arxiv.org/format/1802.04164">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epja/i2018-12476-7">10.1140/epja/i2018-12476-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-efficiency gas target setup for underground experiments, and redetermination of the branching ratio of the 189.5 keV $\mathbf{^{22}Ne(p,纬)^{23}Na}$ resonance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Piatti%2C+D">D. Piatti</a>, <a href="/search/nucl-ex?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/nucl-ex?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/nucl-ex?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/nucl-ex?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/nucl-ex?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/nucl-ex?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/nucl-ex?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/nucl-ex?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/nucl-ex?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Erasmo%2C+G">G. D'Erasmo</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/nucl-ex?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/nucl-ex?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/nucl-ex?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/nucl-ex?searchtype=author&query=Gervino%2C+G">G. Gervino</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1802.04164v1-abstract-short" style="display: inline;"> The experimental study of nuclear reactions of astrophysical interest is greatly facilitated by a low-background, high-luminosity setup. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator offers ultra-low cosmic-ray induced background due to its location deep underground in the Gran Sasso National Laboratory (INFN-LNGS), Italy, and high intensity, 250-500 $渭$A, proton an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04164v1-abstract-full').style.display = 'inline'; document.getElementById('1802.04164v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1802.04164v1-abstract-full" style="display: none;"> The experimental study of nuclear reactions of astrophysical interest is greatly facilitated by a low-background, high-luminosity setup. The Laboratory for Underground Nuclear Astrophysics (LUNA) 400 kV accelerator offers ultra-low cosmic-ray induced background due to its location deep underground in the Gran Sasso National Laboratory (INFN-LNGS), Italy, and high intensity, 250-500 $渭$A, proton and $伪$ ion beams. In order to fully exploit these features, a high-purity, recirculating gas target system for isotopically enriched gases is coupled to a high-efficiency, six-fold optically segmented bismuth germanate (BGO) $纬$-ray detector. The beam intensity is measured with a beam calorimeter with constant temperature gradient. Pressure and temperature measurements have been carried out at several positions along the beam path, and the resultant gas density profile has been determined. Calibrated $纬$-intensity standards and the well-known $E_p$ = 278 keV $\mathrm{^{14}N(p,纬)^{15}O}$ resonance were used to determine the $纬$-ray detection efficiency and to validate the simulation of the target and detector setup. As an example, the recently measured resonance at $E_p$ = 189.5 keV in the $^{22}$Ne(p,$纬$)$^{23}$Na reaction has been investigated with high statistics, and the $纬$-decay branching ratios of the resonance have been determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1802.04164v1-abstract-full').style.display = 'none'; document.getElementById('1802.04164v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 11 figures, accepted in Eur. Phys. Journal A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. A (2018) 54: 44 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1609.05819">arXiv:1609.05819</a> <span> [<a href="https://arxiv.org/pdf/1609.05819">pdf</a>, <a href="https://arxiv.org/format/1609.05819">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.7566/JPSCP.14.021106">10.7566/JPSCP.14.021106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Progress of the Felsenkeller shallow-underground accelerator for nuclear astrophysics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cowan%2C+T+E">T. E. Cowan</a>, <a href="/search/nucl-ex?searchtype=author&query=Grieger%2C+M">M. Grieger</a>, <a href="/search/nucl-ex?searchtype=author&query=Hensel%2C+T">T. Hensel</a>, <a href="/search/nucl-ex?searchtype=author&query=Junghans%2C+A+R">A. R. Junghans</a>, <a href="/search/nucl-ex?searchtype=author&query=Ludwig%2C+F">F. Ludwig</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%BCller%2C+S+E">S. E. M眉ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Rimarzig%2C+B">B. Rimarzig</a>, <a href="/search/nucl-ex?searchtype=author&query=Reinicke%2C+S">S. Reinicke</a>, <a href="/search/nucl-ex?searchtype=author&query=Schulz%2C+S">S. Schulz</a>, <a href="/search/nucl-ex?searchtype=author&query=Schwengner%2C+R">R. Schwengner</a>, <a href="/search/nucl-ex?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/nucl-ex?searchtype=author&query=Sz%C3%BCcs%2C+T">T. Sz眉cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Tak%C3%A1cs%2C+M+P">M. P. Tak谩cs</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+A">A. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wagner%2C+L">L. Wagner</a>, <a href="/search/nucl-ex?searchtype=author&query=Zuber%2C+K">K. Zuber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.05819v1-abstract-short" style="display: inline;"> Low-background experiments with stable ion beams are an important tool for putting the model of stellar hydrogen, helium, and carbon burning on a solid experimental foundation. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso, using a 0.4 MV accelerator. In the present contribution, the status of the project for a higher-energy underground accelerator is rev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05819v1-abstract-full').style.display = 'inline'; document.getElementById('1609.05819v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.05819v1-abstract-full" style="display: none;"> Low-background experiments with stable ion beams are an important tool for putting the model of stellar hydrogen, helium, and carbon burning on a solid experimental foundation. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso, using a 0.4 MV accelerator. In the present contribution, the status of the project for a higher-energy underground accelerator is reviewed. Two tunnels of the Felsenkeller underground site in Dresden, Germany, are currently being refurbished for the installation of a 5 MV high-current Pelletron accelerator. Construction work is on schedule and expected to complete in August 2017. The accelerator will provide intense, 50 uA, beams of 1H+, 4He+, and 12C+ ions, enabling research on astrophysically relevant nuclear reactions with unprecedented sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.05819v1-abstract-full').style.display = 'none'; document.getElementById('1609.05819v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to the Proceedings of Nuclei in the Cosmos XIV, 19-24 June 2016, Niigata/Japan</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/1501.01983">arXiv:1501.01983</a> <span> [<a href="https://arxiv.org/pdf/1501.01983">pdf</a>, <a href="https://arxiv.org/format/1501.01983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> Neutrino-nucleus interactions and the short-range structure of nuclei </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=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiavilla%2C+R">R. Schiavilla</a>, <a href="/search/nucl-ex?searchtype=author&query=Soderberg%2C+M">M. Soderberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Wiringa%2C+R+B">R. B. Wiringa</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="1501.01983v1-abstract-short" style="display: inline;"> Improvements in theoretical modeling of Short Range structures and phenomena, and comparisons with data, will require sustained collaboration between nuclear theorists and neutrino experimentalists. The extensive history of studying this area of nuclear physics in electron- and hadron-scattering experiments, coupled with the transformative capabilities of LArTPCs to identify neutrinos, will provid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.01983v1-abstract-full').style.display = 'inline'; document.getElementById('1501.01983v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1501.01983v1-abstract-full" style="display: none;"> Improvements in theoretical modeling of Short Range structures and phenomena, and comparisons with data, will require sustained collaboration between nuclear theorists and neutrino experimentalists. The extensive history of studying this area of nuclear physics in electron- and hadron-scattering experiments, coupled with the transformative capabilities of LArTPCs to identify neutrinos, will provide a ripe opportunity for new discoveries that will further our understanding of the nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1501.01983v1-abstract-full').style.display = 'none'; document.getElementById('1501.01983v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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/1408.0598">arXiv:1408.0598</a> <span> [<a href="https://arxiv.org/pdf/1408.0598">pdf</a>, <a href="https://arxiv.org/format/1408.0598">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.113.261801">10.1103/PhysRevLett.113.261801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First Measurement of Neutrino and Antineutrino Coherent Charged Pion Production on Argon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Bromberg%2C+C">C. Bromberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Church%2C+E">E. Church</a>, <a href="/search/nucl-ex?searchtype=author&query=Edmunds%2C+D">D. Edmunds</a>, <a href="/search/nucl-ex?searchtype=author&query=Ereditato%2C+A">A. Ereditato</a>, <a href="/search/nucl-ex?searchtype=author&query=Farooq%2C+S">S. Farooq</a>, <a href="/search/nucl-ex?searchtype=author&query=Fleming%2C+B">B. Fleming</a>, <a href="/search/nucl-ex?searchtype=author&query=Greenlee%2C+H">H. Greenlee</a>, <a href="/search/nucl-ex?searchtype=author&query=Hatcher%2C+R">R. Hatcher</a>, <a href="/search/nucl-ex?searchtype=author&query=Horton-Smith%2C+G">G. Horton-Smith</a>, <a href="/search/nucl-ex?searchtype=author&query=James%2C+C">C. James</a>, <a href="/search/nucl-ex?searchtype=author&query=Klein%2C+E">E. Klein</a>, <a href="/search/nucl-ex?searchtype=author&query=Lang%2C+K">K. Lang</a>, <a href="/search/nucl-ex?searchtype=author&query=Laurens%2C+P">P. Laurens</a>, <a href="/search/nucl-ex?searchtype=author&query=Mehdiyev%2C+R">R. Mehdiyev</a>, <a href="/search/nucl-ex?searchtype=author&query=Page%2C+B">B. Page</a>, <a href="/search/nucl-ex?searchtype=author&query=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Partyka%2C+K">K. Partyka</a>, <a href="/search/nucl-ex?searchtype=author&query=Rameika%2C+G">G. Rameika</a>, <a href="/search/nucl-ex?searchtype=author&query=Rebel%2C+B">B. Rebel</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1408.0598v3-abstract-short" style="display: inline;"> We report on the first cross section measurements for charged current coherent pion production by neutrinos and antineutrinos on argon. These measurements are performed using the ArgoNeuT detector exposed to the NuMI beam at Fermilab. The cross sections are measured to be $2.6^{+1.2}_{-1.0}(stat)^{+0.3}_{-0.4}(syst) \times 10^{-38} \textrm{cm}^{2}/\textrm{Ar}$ for neutrinos at a mean energy of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.0598v3-abstract-full').style.display = 'inline'; document.getElementById('1408.0598v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1408.0598v3-abstract-full" style="display: none;"> We report on the first cross section measurements for charged current coherent pion production by neutrinos and antineutrinos on argon. These measurements are performed using the ArgoNeuT detector exposed to the NuMI beam at Fermilab. The cross sections are measured to be $2.6^{+1.2}_{-1.0}(stat)^{+0.3}_{-0.4}(syst) \times 10^{-38} \textrm{cm}^{2}/\textrm{Ar}$ for neutrinos at a mean energy of $9.6$ GeV and $5.5^{+2.6}_{-2.1}(stat)^{+0.6}_{-0.7}(syst) \times 10^{-39} \textrm{cm}^{2}/\textrm{Ar}$ for antineutrinos at a mean energy of $3.6$ GeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1408.0598v3-abstract-full').style.display = 'none'; document.getElementById('1408.0598v3-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-14-258-E </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 113, 261801 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.4261">arXiv:1405.4261</a> <span> [<a href="https://arxiv.org/pdf/1405.4261">pdf</a>, <a href="https://arxiv.org/format/1405.4261">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.90.012008">10.1103/PhysRevD.90.012008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The detection of back-to-back proton pairs in Charged-Current neutrino interactions with the ArgoNeuT detector in the NuMI low energy beam line </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/nucl-ex?searchtype=author&query=Asaadi%2C+J">J. Asaadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Baller%2C+B">B. Baller</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolton%2C+T">T. Bolton</a>, <a href="/search/nucl-ex?searchtype=author&query=Bromberg%2C+C">C. Bromberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Church%2C+E">E. Church</a>, <a href="/search/nucl-ex?searchtype=author&query=Edmunds%2C+D">D. Edmunds</a>, <a href="/search/nucl-ex?searchtype=author&query=Ereditato%2C+A">A. Ereditato</a>, <a href="/search/nucl-ex?searchtype=author&query=Farooq%2C+S">S. Farooq</a>, <a href="/search/nucl-ex?searchtype=author&query=Fleming%2C+B">B. Fleming</a>, <a href="/search/nucl-ex?searchtype=author&query=Greenlee%2C+H">H. Greenlee</a>, <a href="/search/nucl-ex?searchtype=author&query=Horton-Smith%2C+G">G. Horton-Smith</a>, <a href="/search/nucl-ex?searchtype=author&query=James%2C+C">C. James</a>, <a href="/search/nucl-ex?searchtype=author&query=Klein%2C+E">E. Klein</a>, <a href="/search/nucl-ex?searchtype=author&query=Lang%2C+K">K. Lang</a>, <a href="/search/nucl-ex?searchtype=author&query=Laurens%2C+P">P. Laurens</a>, <a href="/search/nucl-ex?searchtype=author&query=Mehdiyev%2C+R">R. Mehdiyev</a>, <a href="/search/nucl-ex?searchtype=author&query=Page%2C+B">B. Page</a>, <a href="/search/nucl-ex?searchtype=author&query=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Partyka%2C+K">K. Partyka</a>, <a href="/search/nucl-ex?searchtype=author&query=Rameika%2C+G">G. Rameika</a>, <a href="/search/nucl-ex?searchtype=author&query=Rebel%2C+B">B. Rebel</a>, <a href="/search/nucl-ex?searchtype=author&query=Soderberg%2C+M">M. Soderberg</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1405.4261v1-abstract-short" style="display: inline;"> Short range nucleon-nucleon correlations in nuclei (NN SRC) carry important information on nuclear structure and dynamics. NN SRC have been extensively probed through two-nucleon knock- out reactions in both pion and electron scattering experiments. We report here on the detection of two-nucleon knock-out events from neutrino interactions and discuss their topological features as possibly involvin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.4261v1-abstract-full').style.display = 'inline'; document.getElementById('1405.4261v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.4261v1-abstract-full" style="display: none;"> Short range nucleon-nucleon correlations in nuclei (NN SRC) carry important information on nuclear structure and dynamics. NN SRC have been extensively probed through two-nucleon knock- out reactions in both pion and electron scattering experiments. We report here on the detection of two-nucleon knock-out events from neutrino interactions and discuss their topological features as possibly involving NN SRC content in the target argon nuclei. The ArgoNeuT detector in the Main Injector neutrino beam at Fermilab has recorded a sample of 30 fully reconstructed charged current events where the leading muon is accompanied by a pair of protons at the interaction vertex, 19 of which have both protons above the Fermi momentum of the Ar nucleus. Out of these 19 events, four are found with the two protons in a strictly back-to-back high momenta configuration directly observed in the final state and can be associated to nucleon Resonance pionless mechanisms involving a pre-existing short range correlated np pair in the nucleus. Another fraction (four events) of the remaining 15 events have a reconstructed back-to-back configuration of a np pair in the initial state, a signature compatible with one-body Quasi Elastic interaction on a neutron in a SRC pair. The detection of these two subsamples of the collected (mu- + 2p) events suggests that mechanisms directly involving nucleon-nucleon SRC pairs in the nucleus are active and can be efficiently explored in neutrino-argon interactions with the LAr TPC technology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.4261v1-abstract-full').style.display = 'none'; document.getElementById('1405.4261v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 90, 012008 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.0125">arXiv:1310.0125</a> <span> [<a href="https://arxiv.org/pdf/1310.0125">pdf</a>, <a href="https://arxiv.org/format/1310.0125">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Coherent Scattering Investigations at the Spallation Neutron Source: a Snowmass White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Akimov%2C+D">D. Akimov</a>, <a href="/search/nucl-ex?searchtype=author&query=Bernstein%2C+A">A. Bernstein</a>, <a href="/search/nucl-ex?searchtype=author&query=Barbeau%2C+P">P. Barbeau</a>, <a href="/search/nucl-ex?searchtype=author&query=Barton%2C+P">P. Barton</a>, <a href="/search/nucl-ex?searchtype=author&query=Bolozdynya%2C+A">A. Bolozdynya</a>, <a href="/search/nucl-ex?searchtype=author&query=Cabrera-Palmer%2C+B">B. Cabrera-Palmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cianciolo%2C+V">V. Cianciolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Collar%2C+J">J. Collar</a>, <a href="/search/nucl-ex?searchtype=author&query=Cooper%2C+R+J">R. J. Cooper</a>, <a href="/search/nucl-ex?searchtype=author&query=Dean%2C+D">D. Dean</a>, <a href="/search/nucl-ex?searchtype=author&query=Efremenko%2C+Y">Y. Efremenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Etenko%2C+A">A. Etenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Fields%2C+N">N. Fields</a>, <a href="/search/nucl-ex?searchtype=author&query=Foxe%2C+M">M. Foxe</a>, <a href="/search/nucl-ex?searchtype=author&query=Figueroa-Feliciano%2C+E">E. Figueroa-Feliciano</a>, <a href="/search/nucl-ex?searchtype=author&query=Fomin%2C+N">N. Fomin</a>, <a href="/search/nucl-ex?searchtype=author&query=Gallmeier%2C+F">F. Gallmeier</a>, <a href="/search/nucl-ex?searchtype=author&query=Garishvili%2C+I">I. Garishvili</a>, <a href="/search/nucl-ex?searchtype=author&query=Gerling%2C+M">M. Gerling</a>, <a href="/search/nucl-ex?searchtype=author&query=Green%2C+M">M. Green</a>, <a href="/search/nucl-ex?searchtype=author&query=Greene%2C+G">G. Greene</a>, <a href="/search/nucl-ex?searchtype=author&query=Hatzikoutelis%2C+A">A. Hatzikoutelis</a>, <a href="/search/nucl-ex?searchtype=author&query=Henning%2C+R">R. Henning</a>, <a href="/search/nucl-ex?searchtype=author&query=Hix%2C+R">R. Hix</a> , et al. (32 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1310.0125v1-abstract-short" style="display: inline;"> The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this white paper, we describe how the SNS source can be used for a measurement of coherent elastic neutrino-nucleus scattering (CENNS), and the physics reach of dif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.0125v1-abstract-full').style.display = 'inline'; document.getElementById('1310.0125v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.0125v1-abstract-full" style="display: none;"> The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this white paper, we describe how the SNS source can be used for a measurement of coherent elastic neutrino-nucleus scattering (CENNS), and the physics reach of different phases of such an experimental program (CSI: Coherent Scattering Investigations at the SNS). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.0125v1-abstract-full').style.display = 'none'; document.getElementById('1310.0125v1-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 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Snowmass white paper</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.5199">arXiv:1211.5199</a> <span> [<a href="https://arxiv.org/pdf/1211.5199">pdf</a>, <a href="https://arxiv.org/format/1211.5199">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Opportunities for Neutrino Physics at the Spallation Neutron Source: A White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bolozdynya%2C+A">A. Bolozdynya</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Efremenko%2C+Y">Y. Efremenko</a>, <a href="/search/nucl-ex?searchtype=author&query=Garvey%2C+G+T">G. T. Garvey</a>, <a href="/search/nucl-ex?searchtype=author&query=Gudkov%2C+V">V. Gudkov</a>, <a href="/search/nucl-ex?searchtype=author&query=Hatzikoutelis%2C+A">A. Hatzikoutelis</a>, <a href="/search/nucl-ex?searchtype=author&query=Hix%2C+W+R">W. R. Hix</a>, <a href="/search/nucl-ex?searchtype=author&query=Louis%2C+W+C">W. C. Louis</a>, <a href="/search/nucl-ex?searchtype=author&query=Link%2C+J+M">J. M. Link</a>, <a href="/search/nucl-ex?searchtype=author&query=Markoff%2C+D+M">D. M. Markoff</a>, <a href="/search/nucl-ex?searchtype=author&query=Mills%2C+G+B">G. B. Mills</a>, <a href="/search/nucl-ex?searchtype=author&query=Patton%2C+K">K. Patton</a>, <a href="/search/nucl-ex?searchtype=author&query=Ray%2C+H">H. Ray</a>, <a href="/search/nucl-ex?searchtype=author&query=Scholberg%2C+K">K. Scholberg</a>, <a href="/search/nucl-ex?searchtype=author&query=Van+de+Water%2C+R+G">R. G. Van de Water</a>, <a href="/search/nucl-ex?searchtype=author&query=Virtue%2C+C">C. Virtue</a>, <a href="/search/nucl-ex?searchtype=author&query=White%2C+D+H">D. H. White</a>, <a href="/search/nucl-ex?searchtype=author&query=Yen%2C+S">S. Yen</a>, <a href="/search/nucl-ex?searchtype=author&query=Yoo%2C+J">J. Yoo</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="1211.5199v1-abstract-short" style="display: inline;"> The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this document, the product of a workshop at the SNS in May 2012, we describe this free, high-quality stopped-pion neutrino source and outline various physics that c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5199v1-abstract-full').style.display = 'inline'; document.getElementById('1211.5199v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.5199v1-abstract-full" style="display: none;"> The Spallation Neutron Source (SNS) at Oak Ridge National Laboratory, Tennessee, provides an intense flux of neutrinos in the few tens-of-MeV range, with a sharply-pulsed timing structure that is beneficial for background rejection. In this document, the product of a workshop at the SNS in May 2012, we describe this free, high-quality stopped-pion neutrino source and outline various physics that could be done using it. We describe without prioritization some specific experimental configurations that could address these physics topics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5199v1-abstract-full').style.display = 'none'; document.getElementById('1211.5199v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">White paper associated with the Workshop on Neutrinos at the Spallation Neutron Source, May 2012</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1204.5379">arXiv:1204.5379</a> <span> [<a href="https://arxiv.org/pdf/1204.5379">pdf</a>, <a href="https://arxiv.org/format/1204.5379">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <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"> Light Sterile Neutrinos: A White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Abazajian%2C+K+N">K. N. Abazajian</a>, <a href="/search/nucl-ex?searchtype=author&query=Acero%2C+M+A">M. A. Acero</a>, <a href="/search/nucl-ex?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/nucl-ex?searchtype=author&query=Aguilar-Arevalo%2C+A+A">A. A. Aguilar-Arevalo</a>, <a href="/search/nucl-ex?searchtype=author&query=Albright%2C+C+H">C. H. Albright</a>, <a href="/search/nucl-ex?searchtype=author&query=Antusch%2C+S">S. Antusch</a>, <a href="/search/nucl-ex?searchtype=author&query=Arguelles%2C+C+A">C. A. Arguelles</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=Barenboim%2C+G">G. Barenboim</a>, <a href="/search/nucl-ex?searchtype=author&query=Barger%2C+V">V. Barger</a>, <a href="/search/nucl-ex?searchtype=author&query=Bernardini%2C+P">P. Bernardini</a>, <a href="/search/nucl-ex?searchtype=author&query=Bezrukov%2C+F">F. Bezrukov</a>, <a href="/search/nucl-ex?searchtype=author&query=Bjaelde%2C+O+E">O. E. Bjaelde</a>, <a href="/search/nucl-ex?searchtype=author&query=Bogacz%2C+S+A">S. A. Bogacz</a>, <a href="/search/nucl-ex?searchtype=author&query=Bowden%2C+N+S">N. S. Bowden</a>, <a href="/search/nucl-ex?searchtype=author&query=Boyarsky%2C+A">A. Boyarsky</a>, <a href="/search/nucl-ex?searchtype=author&query=Bravar%2C+A">A. Bravar</a>, <a href="/search/nucl-ex?searchtype=author&query=Berguno%2C+D+B">D. Bravo Berguno</a>, <a href="/search/nucl-ex?searchtype=author&query=Brice%2C+S+J">S. J. Brice</a>, <a href="/search/nucl-ex?searchtype=author&query=Bross%2C+A+D">A. D. Bross</a>, <a href="/search/nucl-ex?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Chun%2C+E+J">E. J. Chun</a>, <a href="/search/nucl-ex?searchtype=author&query=Cleveland%2C+B+T">B. T. Cleveland</a>, <a href="/search/nucl-ex?searchtype=author&query=Collin%2C+A+P">A. P. Collin</a> , et al. (162 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="1204.5379v1-abstract-short" style="display: inline;"> This white paper addresses the hypothesis of light sterile neutrinos based on recent anomalies observed in neutrino experiments and the latest astrophysical data. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1204.5379v1-abstract-full" style="display: none;"> This white paper addresses the hypothesis of light sterile neutrinos based on recent anomalies observed in neutrino experiments and the latest astrophysical data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.5379v1-abstract-full').style.display = 'none'; document.getElementById('1204.5379v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2012. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1203.1371">arXiv:1203.1371</a> <span> [<a href="https://arxiv.org/pdf/1203.1371">pdf</a>, <a href="https://arxiv.org/format/1203.1371">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <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/10.1088/1748-0221/7/07/P07003">10.1088/1748-0221/7/07/P07003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tests of PMT Signal Read-out of Liquid Argon Scintillation with a New Fast Waveform Digitizer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cortopassi%2C+A">A. Cortopassi</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Incecco%2C+M">M. D'Incecco</a>, <a href="/search/nucl-ex?searchtype=author&query=Mini%2C+G">G. Mini</a>, <a href="/search/nucl-ex?searchtype=author&query=Pietropaolo%2C+F">F. Pietropaolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Romboli%2C+A">A. Romboli</a>, <a href="/search/nucl-ex?searchtype=author&query=Segreto%2C+E">E. Segreto</a>, <a href="/search/nucl-ex?searchtype=author&query=Szelc%2C+A+M">A. M. Szelc</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="1203.1371v2-abstract-short" style="display: inline;"> The CAEN V1751 is a new generation of Waveform Digitizer recently introduced by CAEN SpA. It features 8 Channels per board, 10 bit, 1 GS/s using Flash ADCs Waveform Digitizers (or 4 channels at 2 GS/s in Dual Edge Sampling mode) with threshold and Auto-Trigger capabilities. This provides a good basis for data acquisition in Dark Matter searches using PMTs to detect scintillation light in liquid ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.1371v2-abstract-full').style.display = 'inline'; document.getElementById('1203.1371v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1203.1371v2-abstract-full" style="display: none;"> The CAEN V1751 is a new generation of Waveform Digitizer recently introduced by CAEN SpA. It features 8 Channels per board, 10 bit, 1 GS/s using Flash ADCs Waveform Digitizers (or 4 channels at 2 GS/s in Dual Edge Sampling mode) with threshold and Auto-Trigger capabilities. This provides a good basis for data acquisition in Dark Matter searches using PMTs to detect scintillation light in liquid argon, as it matches the requirements for measuring the fast scintillation component. The board was tested by operating it in real experimental conditions and by comparing it with a state of the art digital oscilloscope. We find that the sampling at 1 or 2 GS/s is appropriate for the reconstruction of the fast component of the scintillation light in argon (characteristic time of about 6-7 ns) and the extended dynamic range, after a small customization, allows for the detection of signals in the range of energy needed. The bandwidth is found to be adequate and the intrinsic noise is very low. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1203.1371v2-abstract-full').style.display = 'none'; document.getElementById('1203.1371v2-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 July, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 March, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Published in Journal of Instrumentation</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2012 JINST 7 P07003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1108.5584">arXiv:1108.5584</a> <span> [<a href="https://arxiv.org/pdf/1108.5584">pdf</a>, <a href="https://arxiv.org/format/1108.5584">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/7/01/P01016">10.1088/1748-0221/7/01/P01016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Demonstration and Comparison of Operation of Photomultiplier Tubes at Liquid Argon Temperature </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/nucl-ex?searchtype=author&query=Boffelli%2C+F">F. Boffelli</a>, <a href="/search/nucl-ex?searchtype=author&query=Cambiaghi%2C+M">M. Cambiaghi</a>, <a href="/search/nucl-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Cocco%2C+A+G">A. G. Cocco</a>, <a href="/search/nucl-ex?searchtype=author&query=Deniskina%2C+N">N. Deniskina</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Pompeo%2C+F">F. Di Pompeo</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiorillo%2C+G">G. Fiorillo</a>, <a href="/search/nucl-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/nucl-ex?searchtype=author&query=Grandi%2C+L">L. Grandi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kryczynski%2C+P">P. Kryczynski</a>, <a href="/search/nucl-ex?searchtype=author&query=Meng%2C+G">G. Meng</a>, <a href="/search/nucl-ex?searchtype=author&query=Montanari%2C+C">C. Montanari</a>, <a href="/search/nucl-ex?searchtype=author&query=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Pandola%2C+L">L. Pandola</a>, <a href="/search/nucl-ex?searchtype=author&query=Perfetto%2C+F">F. Perfetto</a>, <a href="/search/nucl-ex?searchtype=author&query=Mortari%2C+G+B+P">G. B. Piano Mortari</a>, <a href="/search/nucl-ex?searchtype=author&query=Pietropaolo%2C+F">F. Pietropaolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Raselli%2C+G+L">G. L. Raselli</a>, <a href="/search/nucl-ex?searchtype=author&query=Rossella%2C+M">M. Rossella</a>, <a href="/search/nucl-ex?searchtype=author&query=Rubbia%2C+C">C. Rubbia</a>, <a href="/search/nucl-ex?searchtype=author&query=Segreto%2C+E">E. Segreto</a>, <a href="/search/nucl-ex?searchtype=author&query=Szelc%2C+A+M">A. M. Szelc</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1108.5584v2-abstract-short" style="display: inline;"> Liquified noble gases are widely used as a target in direct Dark Matter searches. Signals from scintillation in the liquid, following energy deposition from the recoil nuclei scattered by Dark Matter particles (e.g. WIMPs), should be recorded down to very low energies by photosensors suitably designed to operate at cryogenic temperatures. Liquid Argon based detectors for Dark Matter searches curre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.5584v2-abstract-full').style.display = 'inline'; document.getElementById('1108.5584v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1108.5584v2-abstract-full" style="display: none;"> Liquified noble gases are widely used as a target in direct Dark Matter searches. Signals from scintillation in the liquid, following energy deposition from the recoil nuclei scattered by Dark Matter particles (e.g. WIMPs), should be recorded down to very low energies by photosensors suitably designed to operate at cryogenic temperatures. Liquid Argon based detectors for Dark Matter searches currently implement photo multiplier tubes for signal read-out. In the last few years PMTs with photocathodes operating down to liquid Argon temperatures (87 K) have been specially developed with increasing Quantum Efficiency characteristics. The most recent of these, Hamamatsu Photonics Mod. R11065 with peak QE up to about 35%, has been extensively tested within the R&D program of the WArP Collaboration. During these testes the Hamamatsu PMTs showed superb performance and allowed obtaining a light yield around 7 phel/keVee in a Liquid Argon detector with a photocathodic coverage in the 12% range, sufficient for detection of events down to few keVee of energy deposition. This shows that this new type of PMT is suited for experimental applications, in particular for new direct Dark Matter searches with LAr-based experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1108.5584v2-abstract-full').style.display = 'none'; document.getElementById('1108.5584v2-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 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 August, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2011. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0804.1222">arXiv:0804.1222</a> <span> [<a href="https://arxiv.org/pdf/0804.1222">pdf</a>, <a href="https://arxiv.org/format/0804.1222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/5/05/P05003">10.1088/1748-0221/5/05/P05003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Oxygen contamination in liquid Argon: combined effects on ionization electron charge and scintillation light </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/nucl-ex?searchtype=author&query=Baibussinov%2C+B">B. Baibussinov</a>, <a href="/search/nucl-ex?searchtype=author&query=Baldo-Ceolin%2C+M">M. Baldo-Ceolin</a>, <a href="/search/nucl-ex?searchtype=author&query=Benetti%2C+P">P. Benetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/nucl-ex?searchtype=author&query=Calligarich%2C+E">E. Calligarich</a>, <a href="/search/nucl-ex?searchtype=author&query=Cambiaghi%2C+M">M. Cambiaghi</a>, <a href="/search/nucl-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/nucl-ex?searchtype=author&query=Carbonara%2C+F">F. Carbonara</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Centro%2C+S">S. Centro</a>, <a href="/search/nucl-ex?searchtype=author&query=Cocco%2C+A+G">A. G. Cocco</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Pompeo%2C+F">F. Di Pompeo</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiorillo%2C+G">G. Fiorillo</a>, <a href="/search/nucl-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/nucl-ex?searchtype=author&query=Gallo%2C+V">V. Gallo</a>, <a href="/search/nucl-ex?searchtype=author&query=Grandi%2C+L">L. Grandi</a>, <a href="/search/nucl-ex?searchtype=author&query=Meng%2C+G">G. Meng</a>, <a href="/search/nucl-ex?searchtype=author&query=Modena%2C+I">I. Modena</a>, <a href="/search/nucl-ex?searchtype=author&query=Montanari%2C+C">C. Montanari</a>, <a href="/search/nucl-ex?searchtype=author&query=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Pandola%2C+L">L. Pandola</a>, <a href="/search/nucl-ex?searchtype=author&query=Pietropaolo%2C+F">F. Pietropaolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Raselli%2C+G+L">G. L. Raselli</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="0804.1222v1-abstract-short" style="display: inline;"> A dedicated test of the effects of Oxygen contamination in liquid Argon has been performed at the INFN-Gran Sasso Laboratory (LNGS, Italy) within the WArP R&D program. Two detectors have been used: the WArP 2.3 lt prototype and a small (0.7 lt) dedicated detector, coupled with a system for the injection of controlled amounts of gaseous Oxygen. Purpose of the test with the 0.7 lt detector is to d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.1222v1-abstract-full').style.display = 'inline'; document.getElementById('0804.1222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0804.1222v1-abstract-full" style="display: none;"> A dedicated test of the effects of Oxygen contamination in liquid Argon has been performed at the INFN-Gran Sasso Laboratory (LNGS, Italy) within the WArP R&D program. Two detectors have been used: the WArP 2.3 lt prototype and a small (0.7 lt) dedicated detector, coupled with a system for the injection of controlled amounts of gaseous Oxygen. Purpose of the test with the 0.7 lt detector is to detect the reduction of the long-lived component lifetime of the Argon scintillation light emission at increasing O2 concentration. Data from the WArP prototype are used for determining the behavior of both the ionization electron lifetime and the scintillation long-lived component lifetime during the O2-purification process activated in closed loop during the acquisition run. The electron lifetime measurements allow to infer the O2 content of the Argon and correlate it with the long-lived scintillation lifetime data. The effect of Oxygen contamination on the scintillation light has been thus measured over a wide range of O2 concentration, spanning from about 10^-3 ppm up to about 10 ppm. The rate constant of the light quenching process induced by Oxygen in LAr has been found to be k'(O2)=0.54+-0.03 micros^-1 ppm^-1. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.1222v1-abstract-full').style.display = 'none'; document.getElementById('0804.1222v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 5:P05003,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0804.1217">arXiv:0804.1217</a> <span> [<a href="https://arxiv.org/pdf/0804.1217">pdf</a>, <a href="https://arxiv.org/format/0804.1217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/5/06/P06003">10.1088/1748-0221/5/06/P06003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Effects of Nitrogen contamination in liquid Argon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Acciarri%2C+R">R. Acciarri</a>, <a href="/search/nucl-ex?searchtype=author&query=Antonello%2C+M">M. Antonello</a>, <a href="/search/nucl-ex?searchtype=author&query=Baibussinov%2C+B">B. Baibussinov</a>, <a href="/search/nucl-ex?searchtype=author&query=Baldo-Ceolin%2C+M">M. Baldo-Ceolin</a>, <a href="/search/nucl-ex?searchtype=author&query=Benetti%2C+P">P. Benetti</a>, <a href="/search/nucl-ex?searchtype=author&query=Calaprice%2C+F">F. Calaprice</a>, <a href="/search/nucl-ex?searchtype=author&query=Calligarich%2C+E">E. Calligarich</a>, <a href="/search/nucl-ex?searchtype=author&query=Cambiaghi%2C+M">M. Cambiaghi</a>, <a href="/search/nucl-ex?searchtype=author&query=Canci%2C+N">N. Canci</a>, <a href="/search/nucl-ex?searchtype=author&query=Carbonara%2C+F">F. Carbonara</a>, <a href="/search/nucl-ex?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/nucl-ex?searchtype=author&query=Centro%2C+S">S. Centro</a>, <a href="/search/nucl-ex?searchtype=author&query=Cocco%2C+A+G">A. G. Cocco</a>, <a href="/search/nucl-ex?searchtype=author&query=Di+Pompeo%2C+F">F. Di Pompeo</a>, <a href="/search/nucl-ex?searchtype=author&query=Fiorillo%2C+G">G. Fiorillo</a>, <a href="/search/nucl-ex?searchtype=author&query=Galbiati%2C+C">C. Galbiati</a>, <a href="/search/nucl-ex?searchtype=author&query=Gallo%2C+V">V. Gallo</a>, <a href="/search/nucl-ex?searchtype=author&query=Grandi%2C+L">L. Grandi</a>, <a href="/search/nucl-ex?searchtype=author&query=Meng%2C+G">G. Meng</a>, <a href="/search/nucl-ex?searchtype=author&query=Modena%2C+I">I. Modena</a>, <a href="/search/nucl-ex?searchtype=author&query=Montanari%2C+C">C. Montanari</a>, <a href="/search/nucl-ex?searchtype=author&query=Palamara%2C+O">O. Palamara</a>, <a href="/search/nucl-ex?searchtype=author&query=Pandola%2C+L">L. Pandola</a>, <a href="/search/nucl-ex?searchtype=author&query=Pietropaolo%2C+F">F. Pietropaolo</a>, <a href="/search/nucl-ex?searchtype=author&query=Raselli%2C+G+L">G. L. Raselli</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0804.1217v1-abstract-short" style="display: inline;"> A dedicated test of the effects of Nitrogen contamination in liquid Argon has been performed at the INFN-Gran Sasso Laboratory (LNGS, Italy) within the WArP R&D program. A detector has been designed and assembled for this specific task and connected to a system for the injection of controlled amounts of gaseous Nitrogen into the liquid Argon. Purpose of the test is to detect the reduction of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.1217v1-abstract-full').style.display = 'inline'; document.getElementById('0804.1217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0804.1217v1-abstract-full" style="display: none;"> A dedicated test of the effects of Nitrogen contamination in liquid Argon has been performed at the INFN-Gran Sasso Laboratory (LNGS, Italy) within the WArP R&D program. A detector has been designed and assembled for this specific task and connected to a system for the injection of controlled amounts of gaseous Nitrogen into the liquid Argon. Purpose of the test is to detect the reduction of the Ar scintillation light emission as a function of the amount of the Nitrogen contaminant injected in the Argon volume. A wide concentration range, spanning from about 10^-1 ppm up to about 10^3 ppm, has been explored. Measurements have been done with electrons in the energy range of minimum ionizing particles (gamma-conversion from radioactive sources). Source spectra at different Nitrogen contaminations are analyzed, showing sensitive reduction of the scintillation yield at increasing concentrations. The rate constant of the light quenching process induced by Nitrogen in liquid Ar has been found to be k(N2)=0.11 micros^-1 ppm^-1. Direct PMT signals acquisition at high time resolution by fast Waveform recording allowed to extract with high precision the main characteristics of the scintillation light emission in pure and contaminated LAr. In particular, the decreasing behavior in lifetime and relative amplitude of the slow component is found to be appreciable from O(1 ppm) of Nitrogen concentrations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0804.1217v1-abstract-full').style.display = 'none'; document.getElementById('0804.1217v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 April, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2008. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2010 JINST 5 P06003 </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 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