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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/2411.18969">arXiv:2411.18969</a> <span> [<a href="https://arxiv.org/pdf/2411.18969">pdf</a>, <a href="https://arxiv.org/format/2411.18969">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Towards a new generation of solid total-energy detectors for neutron-capture time-of-flight experiments with intense neutron beams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/physics?searchtype=author&query=Babiano-Suarez%2C+V">V. Babiano-Suarez</a>, <a href="/search/physics?searchtype=author&query=Lerendegui-Marco%2C+J">J. Lerendegui-Marco</a>, <a href="/search/physics?searchtype=author&query=Domingo-Pardo%2C+C">C. Domingo-Pardo</a>, <a href="/search/physics?searchtype=author&query=Ladarescu%2C+I">I. Ladarescu</a>, <a href="/search/physics?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">A. Tarife帽o-Saldivia</a>, <a href="/search/physics?searchtype=author&query=de+la+Fuente-Rosales%2C+G">G. de la Fuente-Rosales</a>, <a href="/search/physics?searchtype=author&query=Gameiro%2C+B">B. Gameiro</a>, <a href="/search/physics?searchtype=author&query=Zaitseva%2C+N">N. Zaitseva</a>, <a href="/search/physics?searchtype=author&query=Alcayne%2C+V">V. Alcayne</a>, <a href="/search/physics?searchtype=author&query=Cano-Ott%2C+D">D. Cano-Ott</a>, <a href="/search/physics?searchtype=author&query=Gonz%C3%A1lez-Romero%2C+E">E. Gonz谩lez-Romero</a>, <a href="/search/physics?searchtype=author&query=Mart%C3%ADnez%2C+T">T. Mart铆nez</a>, <a href="/search/physics?searchtype=author&query=Mendoza%2C+E">E. Mendoza</a>, <a href="/search/physics?searchtype=author&query=de+Rada%2C+A+P">A. P茅rez de Rada</a>, <a href="/search/physics?searchtype=author&query=del+Olmo%2C+J+P">J. Plaza del Olmo</a>, <a href="/search/physics?searchtype=author&query=S%C3%A1nchez-Caballero%2C+A">A. S谩nchez-Caballero</a>, <a href="/search/physics?searchtype=author&query=Casanovas%2C+A">A. Casanovas</a>, <a href="/search/physics?searchtype=author&query=Calvi%C3%B1o%2C+F">F. Calvi帽o</a>, <a href="/search/physics?searchtype=author&query=Valenta%2C+S">S. Valenta</a>, <a href="/search/physics?searchtype=author&query=Aberle%2C+O">O. Aberle</a>, <a href="/search/physics?searchtype=author&query=Altieri%2C+S">S. Altieri</a>, <a href="/search/physics?searchtype=author&query=Amaducci%2C+S">S. Amaducci</a>, <a href="/search/physics?searchtype=author&query=Andrzejewski%2C+J">J. Andrzejewski</a>, <a href="/search/physics?searchtype=author&query=Bacak%2C+M">M. Bacak</a> , et al. (112 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="2411.18969v1-abstract-short" style="display: inline;"> Challenging neutron-capture cross-section measurements of small cross sections and samples with a very limited number of atoms require high-flux time-of-flight facilities. In turn, such facilities need innovative detection setups that are fast, have low sensitivity to neutrons, can quickly recover from the so-called $纬$-flash, and offer the highest possible detection sensitivity. In this paper, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18969v1-abstract-full').style.display = 'inline'; document.getElementById('2411.18969v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.18969v1-abstract-full" style="display: none;"> Challenging neutron-capture cross-section measurements of small cross sections and samples with a very limited number of atoms require high-flux time-of-flight facilities. In turn, such facilities need innovative detection setups that are fast, have low sensitivity to neutrons, can quickly recover from the so-called $纬$-flash, and offer the highest possible detection sensitivity. In this paper, we present several steps toward such advanced systems. Specifically, we describe the performance of a high-sensitivity experimental setup at CERN n\_TOF EAR2. It consists of nine sTED detector modules in a compact cylindrical configuration, two conventional used large-volume C$_{6}$D$_{6}$ detectors, and one LaCl$_{3}$(Ce) detector. The performance of these detection systems is compared using $^{93}$Nb($n$,$纬$) data. We also developed a detailed \textsc{Geant4} Monte Carlo model of the experimental EAR2 setup, which allows for a better understanding of the detector features, including their efficiency determination. This Monte Carlo model has been used for further optimization, thus leading to a new conceptual design of a $纬$ detector array, STAR, based on a deuterated-stilbene crystal array. Finally, the suitability of deuterated-stilbene crystals for the future STAR array is investigaged experimentally utilizing a small stilbene-d12 prototype. The results suggest a similar or superior performance of STAR with respect to other setups based on liquid-scintillators, and allow for additional features such as neutron-gamma discrimination and a higher level of customization capability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.18969v1-abstract-full').style.display = 'none'; document.getElementById('2411.18969v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <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/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?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/2311.01365">arXiv:2311.01365</a> <span> [<a href="https://arxiv.org/pdf/2311.01365">pdf</a>, <a href="https://arxiv.org/format/2311.01365">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Pushing the high count rate limits of scintillation detectors for challenging neutron-capture experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Correa%2C+J+B">J. Balibrea Correa</a>, <a href="/search/physics?searchtype=author&query=Lerendegui-Marco%2C+J">J. Lerendegui-Marco</a>, <a href="/search/physics?searchtype=author&query=Babiano-Suarez%2C+V">V. Babiano-Suarez</a>, <a href="/search/physics?searchtype=author&query=Domingo-Pardo%2C+C">C. Domingo-Pardo</a>, <a href="/search/physics?searchtype=author&query=Ladarescu%2C+I">I. Ladarescu</a>, <a href="/search/physics?searchtype=author&query=Tarife%C3%B1o-Saldivia%2C+A">A. Tarife帽o-Saldivia</a>, <a href="/search/physics?searchtype=author&query=Alcayne%2C+V">V. Alcayne</a>, <a href="/search/physics?searchtype=author&query=Cano-Ott%2C+D">D. Cano-Ott</a>, <a href="/search/physics?searchtype=author&query=Gonz%C3%A1lez-Romero%2C+E">E. Gonz谩lez-Romero</a>, <a href="/search/physics?searchtype=author&query=Mart%C3%ADnez%2C+T">T. Mart铆nez</a>, <a href="/search/physics?searchtype=author&query=Mendoza%2C+E">E. Mendoza</a>, <a href="/search/physics?searchtype=author&query=de+Rada%2C+A+P">A. P茅rez de Rada</a>, <a href="/search/physics?searchtype=author&query=del+Olmo%2C+J+P">J. Plaza del Olmo</a>, <a href="/search/physics?searchtype=author&query=S%C3%A1nchez-Caballero%2C+A">A. S谩nchez-Caballero</a>, <a href="/search/physics?searchtype=author&query=Casanovas%2C+A">A. Casanovas</a>, <a href="/search/physics?searchtype=author&query=Calvi%C3%B1o%2C+F">F. Calvi帽o</a>, <a href="/search/physics?searchtype=author&query=Valenta%2C+S">S. Valenta</a>, <a href="/search/physics?searchtype=author&query=Aberle%2C+O">O. Aberle</a>, <a href="/search/physics?searchtype=author&query=Altieri%2C+S">S. Altieri</a>, <a href="/search/physics?searchtype=author&query=Amaducci%2C+S">S. Amaducci</a>, <a href="/search/physics?searchtype=author&query=Andrzejewski%2C+J">J. Andrzejewski</a>, <a href="/search/physics?searchtype=author&query=Bacak%2C+M">M. Bacak</a>, <a href="/search/physics?searchtype=author&query=Beltrami%2C+C">C. Beltrami</a>, <a href="/search/physics?searchtype=author&query=Bennett%2C+S">S. Bennett</a>, <a href="/search/physics?searchtype=author&query=Bernardes%2C+A+P">A. P. Bernardes</a> , et al. (109 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="2311.01365v1-abstract-short" style="display: inline;"> One of the critical aspects for the accurate determination of neutron capture cross sections when combining time-of-flight and total energy detector techniques is the characterization and control of systematic uncertainties associated to the measuring devices. In this work we explore the most conspicuous effects associated to harsh count rate conditions: dead-time and pile-up effects. Both effects… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01365v1-abstract-full').style.display = 'inline'; document.getElementById('2311.01365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01365v1-abstract-full" style="display: none;"> One of the critical aspects for the accurate determination of neutron capture cross sections when combining time-of-flight and total energy detector techniques is the characterization and control of systematic uncertainties associated to the measuring devices. In this work we explore the most conspicuous effects associated to harsh count rate conditions: dead-time and pile-up effects. Both effects, when not properly treated, can lead to large systematic uncertainties and bias in the determination of neutron cross sections. In the majority of neutron capture measurements carried out at the CERN n\_TOF facility, the detectors of choice are the C$_{6}$D$_{6}$ liquid-based either in form of large-volume cells or recently commissioned sTED detector array, consisting of much smaller-volume modules. To account for the aforementioned effects, we introduce a Monte Carlo model for these detectors mimicking harsh count rate conditions similar to those happening at the CERN n\_TOF 20~m fligth path vertical measuring station. The model parameters are extracted by comparison with the experimental data taken at the same facility during 2022 experimental campaign. We propose a novel methodology to consider both, dead-time and pile-up effects simultaneously for these fast detectors and check the applicability to experimental data from $^{197}$Au($n$,$纬$), including the saturated 4.9~eV resonance which is an important component of normalization for neutron cross section measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01365v1-abstract-full').style.display = 'none'; document.getElementById('2311.01365v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.04443">arXiv:2209.04443</a> <span> [<a href="https://arxiv.org/pdf/2209.04443">pdf</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> <p class="title is-5 mathjax"> The CERN n TOF NEAR station for astrophysics- and application-related neutron activation measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Patronis%2C+N">N. Patronis</a>, <a href="/search/physics?searchtype=author&query=Mengoni%2C+A">A. Mengoni</a>, <a href="/search/physics?searchtype=author&query=Colonna%2C+N">N. Colonna</a>, <a href="/search/physics?searchtype=author&query=Cecchetto%2C+M">M. Cecchetto</a>, <a href="/search/physics?searchtype=author&query=Domingo-Pardo%2C+C">C. Domingo-Pardo</a>, <a href="/search/physics?searchtype=author&query=Aberle%2C+O">O. Aberle</a>, <a href="/search/physics?searchtype=author&query=Lerendegui-Marco%2C+J">J. Lerendegui-Marco</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Stamati%2C+M+E">M. E. Stamati</a>, <a href="/search/physics?searchtype=author&query=Goula%2C+S">S. Goula</a>, <a href="/search/physics?searchtype=author&query=Bernardes%2C+A+P">A. P. Bernardes</a>, <a href="/search/physics?searchtype=author&query=Mastromarco%2C+M">M. Mastromarco</a>, <a href="/search/physics?searchtype=author&query=Manna%2C+A">A. Manna</a>, <a href="/search/physics?searchtype=author&query=Vlastou%2C+R">R. Vlastou</a>, <a href="/search/physics?searchtype=author&query=Massimi%2C+C">C. Massimi</a>, <a href="/search/physics?searchtype=author&query=Calviani%2C+M">M. Calviani</a>, <a href="/search/physics?searchtype=author&query=Alcayne%2C+V">V. Alcayne</a>, <a href="/search/physics?searchtype=author&query=Altieri%2C+S">S. Altieri</a>, <a href="/search/physics?searchtype=author&query=Amaducci%2C+S">S. Amaducci</a>, <a href="/search/physics?searchtype=author&query=Andrzejewski%2C+J">J. Andrzejewski</a>, <a href="/search/physics?searchtype=author&query=Babiano-Suarez%2C+V">V. Babiano-Suarez</a>, <a href="/search/physics?searchtype=author&query=Bacak%2C+M">M. Bacak</a>, <a href="/search/physics?searchtype=author&query=Balibrea%2C+J">J. Balibrea</a>, <a href="/search/physics?searchtype=author&query=Beltrami%2C+C">C. Beltrami</a>, <a href="/search/physics?searchtype=author&query=Bennett%2C+S">S. Bennett</a> , et al. (108 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="2209.04443v1-abstract-short" style="display: inline;"> A new experimental area, the NEAR station, has recently been built at the CERN n TOF facility, at a short distance from the spallation target (1.5 m). The new area, characterized by a neutron beam of very high flux, has been designed with the purpose of performing activation measurements of interest for astrophysics and various applications. The beam is transported from the spallation target to th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04443v1-abstract-full').style.display = 'inline'; document.getElementById('2209.04443v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.04443v1-abstract-full" style="display: none;"> A new experimental area, the NEAR station, has recently been built at the CERN n TOF facility, at a short distance from the spallation target (1.5 m). The new area, characterized by a neutron beam of very high flux, has been designed with the purpose of performing activation measurements of interest for astrophysics and various applications. The beam is transported from the spallation target to the NEAR station through a hole in the shielding wall of the target, inside which a collimator is inserted. The new area is complemented with a 纬-ray spectroscopy laboratory, the GEAR station, equipped with a high efficiency HPGe detector, for the measurement of the activity resulting from irradiation of a sample in the NEAR station. The use of a moderator/filter assembly is envisaged, in order to produce a neutron beam of Maxwellian shape at different thermal energies, necessary for the measurement of Maxwellian Averaged Cross Sections of astrophysical interest. A new fast-cycling activation technique is also being investigated, for measurements of reactions leading to isotopes of very short half life. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04443v1-abstract-full').style.display = 'none'; document.getElementById('2209.04443v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </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/physics?searchtype=author&query=Mossa%2C+V">V. Mossa</a>, <a href="/search/physics?searchtype=author&query=St%C3%B6ckel%2C+K">K. St枚ckel</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?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/physics?searchtype=author&query=Ciani%2C+G+F">G. F. Ciani</a>, <a href="/search/physics?searchtype=author&query=Csedreki%2C+L">L. Csedreki</a>, <a href="/search/physics?searchtype=author&query=Balibrea-Correa%2C+J">J. Balibrea-Correa</a>, <a href="/search/physics?searchtype=author&query=Best%2C+A">A. Best</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Barile%2C+F">F. Barile</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Boeltzig%2C+A">A. Boeltzig</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Chillery%2C+T">T. Chillery</a>, <a href="/search/physics?searchtype=author&query=Colombetti%2C+P">P. Colombetti</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Di+Leva%2C+A">A. Di Leva</a>, <a href="/search/physics?searchtype=author&query=Di+Paolo%2C+L">L. Di Paolo</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Fiore%2C+E+M">E. M. Fiore</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=Fulop%2C+Z">Zs. Fulop</a>, <a href="/search/physics?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/1910.11939">arXiv:1910.11939</a> <span> [<a href="https://arxiv.org/pdf/1910.11939">pdf</a>, <a href="https://arxiv.org/format/1910.11939">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/s10050-020-00107-x">10.1140/epja/s10050-020-00107-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The BGOOD experimental setup at ELSA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Alef%2C+S">S. Alef</a>, <a href="/search/physics?searchtype=author&query=Bauer%2C+P">P. Bauer</a>, <a href="/search/physics?searchtype=author&query=Bayadilov%2C+D">D. Bayadilov</a>, <a href="/search/physics?searchtype=author&query=Beck%2C+R">R. Beck</a>, <a href="/search/physics?searchtype=author&query=Becker%2C+M">M. Becker</a>, <a href="/search/physics?searchtype=author&query=Bella%2C+A">A. Bella</a>, <a href="/search/physics?searchtype=author&query=Bieling%2C+J">J. Bieling</a>, <a href="/search/physics?searchtype=author&query=Boese%2C+S">S. Boese</a>, <a href="/search/physics?searchtype=author&query=Braghieri%2C+A">A. Braghieri</a>, <a href="/search/physics?searchtype=author&query=Brinkmann%2C+K+-">K. -Th. Brinkmann</a>, <a href="/search/physics?searchtype=author&query=Cole%2C+P">P. Cole</a>, <a href="/search/physics?searchtype=author&query=Di+Salvo%2C+R">R. Di Salvo</a>, <a href="/search/physics?searchtype=author&query=Elsner%2C+D">D. Elsner</a>, <a href="/search/physics?searchtype=author&query=Fantini%2C+A">A. Fantini</a>, <a href="/search/physics?searchtype=author&query=Freyermuth%2C+O">O. Freyermuth</a>, <a href="/search/physics?searchtype=author&query=Frommberger%2C+F">F. Frommberger</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Ghio%2C+F">F. Ghio</a>, <a href="/search/physics?searchtype=author&query=Goertz%2C+S">S. Goertz</a>, <a href="/search/physics?searchtype=author&query=Gridnev%2C+A">A. Gridnev</a>, <a href="/search/physics?searchtype=author&query=Gutz%2C+E">E. Gutz</a>, <a href="/search/physics?searchtype=author&query=Hammann%2C+D">D. Hammann</a>, <a href="/search/physics?searchtype=author&query=Hannappel%2C+J">J. Hannappel</a>, <a href="/search/physics?searchtype=author&query=Hillert%2C+W">W. Hillert</a>, <a href="/search/physics?searchtype=author&query=Jahn%2C+O">O. Jahn</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1910.11939v3-abstract-short" style="display: inline;"> The BGOOD experiment at the ELSA facility in Bonn has been commissioned within the framework of an international collaboration. The experiment pursues a systematic investigation of non-strange and strange meson photoproduction, in particular $t$-channel processes at low momentum transfer. The setup uniquely combines a central almost $4蟺$ acceptance BGO crystal calorimeter with a large aperture for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11939v3-abstract-full').style.display = 'inline'; document.getElementById('1910.11939v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1910.11939v3-abstract-full" style="display: none;"> The BGOOD experiment at the ELSA facility in Bonn has been commissioned within the framework of an international collaboration. The experiment pursues a systematic investigation of non-strange and strange meson photoproduction, in particular $t$-channel processes at low momentum transfer. The setup uniquely combines a central almost $4蟺$ acceptance BGO crystal calorimeter with a large aperture forward magnetic spectrometer providing excellent detection of both neutral and charged particles, complementary to other setups such as Crystal Barrel, Crystal Ball, LEPS and CLAS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1910.11939v3-abstract-full').style.display = 'none'; document.getElementById('1910.11939v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 37 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 (2020) 56:104 </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/physics?searchtype=author&query=Cavanna%2C+F">F. Cavanna</a>, <a href="/search/physics?searchtype=author&query=Depalo%2C+R">R. Depalo</a>, <a href="/search/physics?searchtype=author&query=Menzel%2C+M+-">M. -L. Menzel</a>, <a href="/search/physics?searchtype=author&query=Aliotta%2C+M">M. Aliotta</a>, <a href="/search/physics?searchtype=author&query=Anders%2C+M">M. Anders</a>, <a href="/search/physics?searchtype=author&query=Bemmerer%2C+D">D. Bemmerer</a>, <a href="/search/physics?searchtype=author&query=Broggini%2C+C">C. Broggini</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+C+G">C. G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Caciolli%2C+A">A. Caciolli</a>, <a href="/search/physics?searchtype=author&query=Corvisiero%2C+P">P. Corvisiero</a>, <a href="/search/physics?searchtype=author&query=Davinson%2C+T">T. Davinson</a>, <a href="/search/physics?searchtype=author&query=di+Leva%2C+A">A. di Leva</a>, <a href="/search/physics?searchtype=author&query=Elekes%2C+Z">Z. Elekes</a>, <a href="/search/physics?searchtype=author&query=Ferraro%2C+F">F. Ferraro</a>, <a href="/search/physics?searchtype=author&query=Formicola%2C+A">A. Formicola</a>, <a href="/search/physics?searchtype=author&query=F%C3%BCl%C3%B6p%2C+Z">Zs. F眉l枚p</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Guglielmetti%2C+A">A. Guglielmetti</a>, <a href="/search/physics?searchtype=author&query=Gustavino%2C+C">C. Gustavino</a>, <a href="/search/physics?searchtype=author&query=Gy%C3%BCrky%2C+G">Gy. Gy眉rky</a>, <a href="/search/physics?searchtype=author&query=Imbriani%2C+G">G. Imbriani</a>, <a href="/search/physics?searchtype=author&query=Junker%2C+M">M. Junker</a>, <a href="/search/physics?searchtype=author&query=Menegazzo%2C+R">R. Menegazzo</a>, <a href="/search/physics?searchtype=author&query=Prati%2C+P">P. Prati</a>, <a href="/search/physics?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/1005.5230">arXiv:1005.5230</a> <span> [<a href="https://arxiv.org/pdf/1005.5230">pdf</a>, <a href="https://arxiv.org/ps/1005.5230">ps</a>, <a href="https://arxiv.org/format/1005.5230">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="Atomic Physics">physics.atom-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.104.241601">10.1103/PhysRevLett.104.241601 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on light-speed anisotropies from Compton scattering of high-energy electrons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bocquet%2C+J+-">J. -P. Bocquet</a>, <a href="/search/physics?searchtype=author&query=Moricciani%2C+D">D. Moricciani</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+V">V. Bellini</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Casano%2C+L">L. Casano</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+A">A. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Di+Salvo%2C+R">R. Di Salvo</a>, <a href="/search/physics?searchtype=author&query=Fantini%2C+A">A. Fantini</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Ghio%2C+F">F. Ghio</a>, <a href="/search/physics?searchtype=author&query=Giardina%2C+G">G. Giardina</a>, <a href="/search/physics?searchtype=author&query=Girolami%2C+B">B. Girolami</a>, <a href="/search/physics?searchtype=author&query=Giusa%2C+A">A. Giusa</a>, <a href="/search/physics?searchtype=author&query=Gurzadyan%2C+V+G">V. G. Gurzadyan</a>, <a href="/search/physics?searchtype=author&query=Kashin%2C+A">A. Kashin</a>, <a href="/search/physics?searchtype=author&query=Knyazyan%2C+S">S. Knyazyan</a>, <a href="/search/physics?searchtype=author&query=Lapik%2C+A">A. Lapik</a>, <a href="/search/physics?searchtype=author&query=Lehnert%2C+R">R. Lehnert</a>, <a href="/search/physics?searchtype=author&query=Sandri%2C+P+L">P. Levi Sandri</a>, <a href="/search/physics?searchtype=author&query=Lleres%2C+A">A. Lleres</a>, <a href="/search/physics?searchtype=author&query=Mammoliti%2C+F">F. Mammoliti</a>, <a href="/search/physics?searchtype=author&query=Mandaglio%2C+G">G. Mandaglio</a>, <a href="/search/physics?searchtype=author&query=Manganaro%2C+M">M. Manganaro</a>, <a href="/search/physics?searchtype=author&query=Margarian%2C+A">A. Margarian</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1005.5230v2-abstract-short" style="display: inline;"> The possibility of anisotropies in the speed of light relative to the limiting speed of electrons is considered. The absence of sidereal variations in the energy of Compton-edge photons at the ESRF's GRAAL facility constrains such anisotropies representing the first non-threshold collision-kinematics study of Lorentz violation. When interpreted within the minimal Standard-Model Extension, this res… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.5230v2-abstract-full').style.display = 'inline'; document.getElementById('1005.5230v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1005.5230v2-abstract-full" style="display: none;"> The possibility of anisotropies in the speed of light relative to the limiting speed of electrons is considered. The absence of sidereal variations in the energy of Compton-edge photons at the ESRF's GRAAL facility constrains such anisotropies representing the first non-threshold collision-kinematics study of Lorentz violation. When interpreted within the minimal Standard-Model Extension, this result yields the two-sided limit of 1.6 x 10^{-14} at 95% confidence level on a combination of the parity-violating photon and electron coefficients kappa_{o+} and c. This new constraint provides an improvement over previous bounds by one order of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.5230v2-abstract-full').style.display = 'none'; document.getElementById('1005.5230v2-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 June, 2010; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 May, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.104:241601,2010 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1004.2867">arXiv:1004.2867</a> <span> [<a href="https://arxiv.org/pdf/1004.2867">pdf</a>, <a href="https://arxiv.org/ps/1004.2867">ps</a>, <a href="https://arxiv.org/format/1004.2867">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1142/9789814374552_0255">10.1142/9789814374552_0255 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new limit on the light speed isotropy from the GRAAL experiment at the ESRF </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gurzadyan%2C+V+G">V. G. Gurzadyan</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+V">V. Bellini</a>, <a href="/search/physics?searchtype=author&query=Beretta%2C+M">M. Beretta</a>, <a href="/search/physics?searchtype=author&query=Bocquet%2C+J+-">J. -P. Bocquet</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+A">A. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Di+Salvo%2C+R">R. Di Salvo</a>, <a href="/search/physics?searchtype=author&query=Fantini%2C+A">A. Fantini</a>, <a href="/search/physics?searchtype=author&query=Franco%2C+D">D. Franco</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Giardina%2C+G">G. Giardina</a>, <a href="/search/physics?searchtype=author&query=Ghio%2C+F">F. Ghio</a>, <a href="/search/physics?searchtype=author&query=Girolami%2C+B">B. Girolami</a>, <a href="/search/physics?searchtype=author&query=Giusa%2C+A">A. Giusa</a>, <a href="/search/physics?searchtype=author&query=Kashin%2C+A">A. Kashin</a>, <a href="/search/physics?searchtype=author&query=Khachatryan%2C+H+G">H. G. Khachatryan</a>, <a href="/search/physics?searchtype=author&query=Knyazyan%2C+S">S. Knyazyan</a>, <a href="/search/physics?searchtype=author&query=Lapik%2C+A">A. Lapik</a>, <a href="/search/physics?searchtype=author&query=Sandri%2C+P+L">P. Levi Sandri</a>, <a href="/search/physics?searchtype=author&query=Lleres%2C+A">A. Lleres</a>, <a href="/search/physics?searchtype=author&query=Mammoliti%2C+F">F. Mammoliti</a>, <a href="/search/physics?searchtype=author&query=Mandaglio%2C+G">G. Mandaglio</a>, <a href="/search/physics?searchtype=author&query=Manganaro%2C+M">M. Manganaro</a>, <a href="/search/physics?searchtype=author&query=Margarian%2C+A">A. Margarian</a>, <a href="/search/physics?searchtype=author&query=Mehrabyan%2C+S">S. Mehrabyan</a>, <a href="/search/physics?searchtype=author&query=Messi%2C+R">R. Messi</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="1004.2867v1-abstract-short" style="display: inline;"> When the electrons stored in the ring of the European Synchrotron Radiation Facility (ESRF, Grenoble) scatter on a laser beam (Compton scattering in flight) the lower energy of the scattered electron spectra, the Compton Edge (CE), is given by the two body photon-electron relativistic kinematics and depends on the velocity of light. A precision measurement of the position of this CE as a function… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.2867v1-abstract-full').style.display = 'inline'; document.getElementById('1004.2867v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1004.2867v1-abstract-full" style="display: none;"> When the electrons stored in the ring of the European Synchrotron Radiation Facility (ESRF, Grenoble) scatter on a laser beam (Compton scattering in flight) the lower energy of the scattered electron spectra, the Compton Edge (CE), is given by the two body photon-electron relativistic kinematics and depends on the velocity of light. A precision measurement of the position of this CE as a function of the daily variations of the direction of the electron beam in an absolute reference frame provides a one-way test of Relativistic Kinematics and the isotropy of the velocity of light. The results of GRAAL-ESRF measurements improve the previously existing one-way limits, thus showing the efficiency of this method and the interest of further studies in this direction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1004.2867v1-abstract-full').style.display = 'none'; document.getElementById('1004.2867v1-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 April, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceed. MG12 meeting, Paris, July, 2009</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0701127">arXiv:astro-ph/0701127</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0701127">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0701127">ps</a>, <a href="https://arxiv.org/format/astro-ph/0701127">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1393/ncb/i2007-10393-7">10.1393/ncb/i2007-10393-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lowering the Light Speed Isotropy Limit: European Synchrotron Radiation Facility Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gurzadyan%2C+V+G">V. G. Gurzadyan</a>, <a href="/search/physics?searchtype=author&query=Bocquet%2C+J+-">J. -P. Bocquet</a>, <a href="/search/physics?searchtype=author&query=Kashin%2C+A">A. Kashin</a>, <a href="/search/physics?searchtype=author&query=Margarian%2C+A">A. Margarian</a>, <a href="/search/physics?searchtype=author&query=Bartalini%2C+O">O. Bartalini</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+V">V. Bellini</a>, <a href="/search/physics?searchtype=author&query=Castoldi%2C+M">M. Castoldi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+A">A. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Didelez%2C+J+-">J. -P. Didelez</a>, <a href="/search/physics?searchtype=author&query=Di+Salvo%2C+R">R. Di Salvo</a>, <a href="/search/physics?searchtype=author&query=Fantini%2C+A">A. Fantini</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Ghio%2C+F">F. Ghio</a>, <a href="/search/physics?searchtype=author&query=Girolami%2C+B">B. Girolami</a>, <a href="/search/physics?searchtype=author&query=Giusa%2C+A">A. Giusa</a>, <a href="/search/physics?searchtype=author&query=Guidal%2C+M">M. Guidal</a>, <a href="/search/physics?searchtype=author&query=Hourany%2C+E">E. Hourany</a>, <a href="/search/physics?searchtype=author&query=Knyazyan%2C+S">S. Knyazyan</a>, <a href="/search/physics?searchtype=author&query=Kouznetsov%2C+V">V. Kouznetsov</a>, <a href="/search/physics?searchtype=author&query=Kunne%2C+R">R. Kunne</a>, <a href="/search/physics?searchtype=author&query=Lapik%2C+A">A. Lapik</a>, <a href="/search/physics?searchtype=author&query=Sandri%2C+P+L">P. Levi Sandri</a>, <a href="/search/physics?searchtype=author&query=Lleres%2C+A">A. Lleres</a>, <a href="/search/physics?searchtype=author&query=Mehrabyan%2C+S">S. Mehrabyan</a>, <a href="/search/physics?searchtype=author&query=Moricciani%2C+D">D. Moricciani</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="astro-ph/0701127v2-abstract-short" style="display: inline;"> The measurement of the Compton edge of the scattered electrons in GRAAL facility in European Synchrotron Radiation Facility (ESRF) in Grenoble with respect to the Cosmic Microwave Background dipole reveals up to 10 sigma variations larger than the statistical errors. We now show that the variations are not due to the frequency variations of the accelerator. The nature of Compton edge variations… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0701127v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0701127v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0701127v2-abstract-full" style="display: none;"> The measurement of the Compton edge of the scattered electrons in GRAAL facility in European Synchrotron Radiation Facility (ESRF) in Grenoble with respect to the Cosmic Microwave Background dipole reveals up to 10 sigma variations larger than the statistical errors. We now show that the variations are not due to the frequency variations of the accelerator. The nature of Compton edge variations remains unclear, thus outlining the imperative of dedicated studies of light speed anisotropy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0701127v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0701127v2-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 May, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Il Nuovo Cimento, B122 (2007) 515 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/physics/0512182">arXiv:physics/0512182</a> <span> [<a href="https://arxiv.org/pdf/physics/0512182">pdf</a>, <a href="https://arxiv.org/ps/physics/0512182">ps</a>, <a href="https://arxiv.org/format/physics/0512182">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Classical Physics">physics.class-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjb/e2006-00060-x">10.1140/epjb/e2006-00060-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Thermoeconomic analysis of an irreversible Stirling heat pump cycle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Lucia%2C+U">U. Lucia</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</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="physics/0512182v1-abstract-short" style="display: inline;"> In this paper an analysis of the Stirling cycle in thermoeconomic terms is developed using the entropy generation. In the thermoeconomic optimization of an irreversible Stirling heat pump cycle the F function has been introduced to evaluate the optimum for the higher and lower sources temperature ratio in the cycle: this ratio represents the value which optimizes the cycle itself. The variation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0512182v1-abstract-full').style.display = 'inline'; document.getElementById('physics/0512182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="physics/0512182v1-abstract-full" style="display: none;"> In this paper an analysis of the Stirling cycle in thermoeconomic terms is developed using the entropy generation. In the thermoeconomic optimization of an irreversible Stirling heat pump cycle the F function has been introduced to evaluate the optimum for the higher and lower sources temperature ratio in the cycle: this ratio represents the value which optimizes the cycle itself. The variation of the function F is proportional to the variation of the entropy generation, the maxima and minima of F has been evaluated in a previous paper without giving the physical foundation of the method. We investigate the groundwork of this approach: to study the upper and lower limits of F function allows to determine the cycle stability and the optimization conditions. The optimization consists in the best COP at the least cost. The principle of maximum variation for the entropy generation becomes the analytic foundation of the optimization method in the thermoeconomic analysis for an irreversible Stirling heat pump cycle. Pacs: 89.65.G, 05.70 keywords: entropy generation, finite time Thermodynamics, Stirling cycle, Thermodynamic optimization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/0512182v1-abstract-full').style.display = 'none'; document.getElementById('physics/0512182v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, presented to the International Conference NEXT2005, Creta, August 2005</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur Phys Jnl B 50 367-369 (2006) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0410742">arXiv:astro-ph/0410742</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0410742">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0410742">ps</a>, <a href="https://arxiv.org/format/astro-ph/0410742">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1142/S0217732305016294">10.1142/S0217732305016294 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the Light Speed Anisotropy with respect to the Cosmic Microwave Background Radiation Dipole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gurzadyan%2C+V+G">V. G. Gurzadyan</a>, <a href="/search/physics?searchtype=author&query=Bocquet%2C+J+-">J. -P. Bocquet</a>, <a href="/search/physics?searchtype=author&query=Kashin%2C+A">A. Kashin</a>, <a href="/search/physics?searchtype=author&query=Margarian%2C+A">A. Margarian</a>, <a href="/search/physics?searchtype=author&query=Bartalini%2C+O">O. Bartalini</a>, <a href="/search/physics?searchtype=author&query=Bellini%2C+V">V. Bellini</a>, <a href="/search/physics?searchtype=author&query=Castoldi%2C+M">M. Castoldi</a>, <a href="/search/physics?searchtype=author&query=D%27Angelo%2C+A">A. D'Angelo</a>, <a href="/search/physics?searchtype=author&query=Didelez%2C+J+-">J. -P. Didelez</a>, <a href="/search/physics?searchtype=author&query=Di+Salvo%2C+R">R. Di Salvo</a>, <a href="/search/physics?searchtype=author&query=Fantini%2C+A">A. Fantini</a>, <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Ghio%2C+F">F. Ghio</a>, <a href="/search/physics?searchtype=author&query=Girolami%2C+B">B. Girolami</a>, <a href="/search/physics?searchtype=author&query=Giusa%2C+A">A. Giusa</a>, <a href="/search/physics?searchtype=author&query=Guidal%2C+M">M. Guidal</a>, <a href="/search/physics?searchtype=author&query=Hourany%2C+E">E. Hourany</a>, <a href="/search/physics?searchtype=author&query=Knyazyan%2C+S">S. Knyazyan</a>, <a href="/search/physics?searchtype=author&query=Kouznetsov%2C+V">V. Kouznetsov</a>, <a href="/search/physics?searchtype=author&query=Kunne%2C+R">R. Kunne</a>, <a href="/search/physics?searchtype=author&query=Lapik%2C+A">A. Lapik</a>, <a href="/search/physics?searchtype=author&query=Sandri%2C+P+L">P. Levi Sandri</a>, <a href="/search/physics?searchtype=author&query=Lleres%2C+A">A. Lleres</a>, <a href="/search/physics?searchtype=author&query=Mehrabyan%2C+S">S. Mehrabyan</a>, <a href="/search/physics?searchtype=author&query=Moricciani%2C+D">D. Moricciani</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="astro-ph/0410742v2-abstract-short" style="display: inline;"> We have studied the angular fluctuations in the speed of light with respect to the apex of the dipole of Cosmic Microwave Background (CMB) radiation using the experimental data obtained with GRAAL facility, located at the European Synchrotron Radiation Facility (ESRF) in Grenoble. The measurements were based on the stability of the Compton edge of laser photons scattered on the 6 GeV monochromat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0410742v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0410742v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0410742v2-abstract-full" style="display: none;"> We have studied the angular fluctuations in the speed of light with respect to the apex of the dipole of Cosmic Microwave Background (CMB) radiation using the experimental data obtained with GRAAL facility, located at the European Synchrotron Radiation Facility (ESRF) in Grenoble. The measurements were based on the stability of the Compton edge of laser photons scattered on the 6 GeV monochromatic electron beam. The results enable to obtain a conservative constraint on the anisotropy in the light speed variations 螖c(胃)/c < 3 10^{-12}, i.e. with higher precision than from previous experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0410742v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0410742v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2005; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 October, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2004. </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">The published version: reported at the workshop "Testing the Equivalence Principle in Space and on Ground" (STEP), Pescara, Italy, September, 2004</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mod.Phys.Lett. A20 (2005) 19-28 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/physics/9809001">arXiv:physics/9809001</a> <span> [<a href="https://arxiv.org/pdf/physics/9809001">pdf</a>, <a href="https://arxiv.org/ps/physics/9809001">ps</a>, <a href="https://arxiv.org/format/physics/9809001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Non-Markovian effects in the solar neutrino problem </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Gervino%2C+G">G. Gervino</a>, <a href="/search/physics?searchtype=author&query=Kaniadakis%2C+G">G. Kaniadakis</a>, <a href="/search/physics?searchtype=author&query=Lavagno%2C+A">A. Lavagno</a>, <a href="/search/physics?searchtype=author&query=Lissia%2C+M">M. Lissia</a>, <a href="/search/physics?searchtype=author&query=Quarati%2C+P">P. Quarati</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="physics/9809001v1-abstract-short" style="display: inline;"> The solar core, because of its density and temperature, is not a weakly-interacting or a high-temperature plasma. Collective effects have time scales comparable to the average time between collisions, and the microfield distribution influences the particle dynamics. In this conditions ion and electron diffusion is a non-Markovian process, memory effects are present and the equilibrium statistica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/9809001v1-abstract-full').style.display = 'inline'; document.getElementById('physics/9809001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="physics/9809001v1-abstract-full" style="display: none;"> The solar core, because of its density and temperature, is not a weakly-interacting or a high-temperature plasma. Collective effects have time scales comparable to the average time between collisions, and the microfield distribution influences the particle dynamics. In this conditions ion and electron diffusion is a non-Markovian process, memory effects are present and the equilibrium statistical distribution function differs from the Maxwellian one. We show that, even if the deviations from the standard velocity distribution that are compatible with our present knowledge of the solar interior are small, they are sufficient to sensibly modify the sub-barrier nuclear reaction rates. The consequent changes of the neutrino fluxes are comparable to the flux deficits that constitute the solar neutrino problem. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('physics/9809001v1-abstract-full').style.display = 'none'; document.getElementById('physics/9809001v1-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 September, 1998; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1998. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, to appear in the Proceedings of Nuclei in the Cosmos V</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> INFNCA-TH9810 </p> </li> </ol> <div class="is-hidden-tablet">  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