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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/2412.01723">arXiv:2412.01723</a> <span> [<a href="https://arxiv.org/pdf/2412.01723">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41467-024-54040-4">10.1038/s41467-024-54040-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enhanced production of 60Fe in massive stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Spyrou%2C+A">A. Spyrou</a>, <a href="/search/nucl-ex?searchtype=author&query=Richman%2C+D">D. Richman</a>, <a href="/search/nucl-ex?searchtype=author&query=Couture%2C+A">A. Couture</a>, <a href="/search/nucl-ex?searchtype=author&query=Fields%2C+C+E">C. E. Fields</a>, <a href="/search/nucl-ex?searchtype=author&query=Liddick%2C+S+N">S. N. Liddick</a>, <a href="/search/nucl-ex?searchtype=author&query=Childers%2C+K">K. Childers</a>, <a href="/search/nucl-ex?searchtype=author&query=Crider%2C+B+P">B. P. Crider</a>, <a href="/search/nucl-ex?searchtype=author&query=DeYoung%2C+P+A">P. A. DeYoung</a>, <a href="/search/nucl-ex?searchtype=author&query=Dombos%2C+A+C">A. C. Dombos</a>, <a href="/search/nucl-ex?searchtype=author&query=Gastis%2C+P">P. Gastis</a>, <a href="/search/nucl-ex?searchtype=author&query=Guttormsen%2C+M">M. Guttormsen</a>, <a href="/search/nucl-ex?searchtype=author&query=Hermansen%2C+K">K. Hermansen</a>, <a href="/search/nucl-ex?searchtype=author&query=Larsen%2C+A+C">A. C. Larsen</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Lyons%2C+S">S. Lyons</a>, <a href="/search/nucl-ex?searchtype=author&query=Midtb%C3%B8%2C+J+E">J. E. Midtb酶</a>, <a href="/search/nucl-ex?searchtype=author&query=Mosby%2C+S">S. Mosby</a>, <a href="/search/nucl-ex?searchtype=author&query=Muecher%2C+D">D. Muecher</a>, <a href="/search/nucl-ex?searchtype=author&query=Naqvi%2C+F">F. Naqvi</a>, <a href="/search/nucl-ex?searchtype=author&query=Palmisano-Kyle%2C+A">A. Palmisano-Kyle</a>, <a href="/search/nucl-ex?searchtype=author&query=Perdikakis%2C+G">G. Perdikakis</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokop%2C+C">C. Prokop</a>, <a href="/search/nucl-ex?searchtype=author&query=Schatz%2C+H">H. Schatz</a>, <a href="/search/nucl-ex?searchtype=author&query=Smith%2C+M+K">M. K. Smith</a>, <a href="/search/nucl-ex?searchtype=author&query=Sumithrarachchi%2C+C">C. Sumithrarachchi</a> , et al. (1 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="2412.01723v1-abstract-short" style="display: inline;"> Massive stars are a major source of chemical elements in the cosmos, ejecting freshly produced nuclei through winds and core-collapse supernova explosions into the interstellar medium. Among the material ejected, long lived radioisotopes, such as 60Fe (iron) and 26Al (aluminum), offer unique signs of active nucleosynthesis in our galaxy. There is a long-standing discrepancy between the observed 60… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01723v1-abstract-full').style.display = 'inline'; document.getElementById('2412.01723v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.01723v1-abstract-full" style="display: none;"> Massive stars are a major source of chemical elements in the cosmos, ejecting freshly produced nuclei through winds and core-collapse supernova explosions into the interstellar medium. Among the material ejected, long lived radioisotopes, such as 60Fe (iron) and 26Al (aluminum), offer unique signs of active nucleosynthesis in our galaxy. There is a long-standing discrepancy between the observed 60Fe/26Al ratio by 纬-ray telescopes and predictions from supernova models. This discrepancy has been attributed to uncertainties in the nuclear reaction networks producing 60Fe, and one reaction in particular, the neutron-capture on 59Fe. Here we present experimental results that provide a strong constraint on this reaction. We use these results to show that the production of 60Fe in massive stars is higher than previously thought, further increasing the discrepancy between observed and predicted 60Fe/26Al ratios. The persisting discrepancy can therefore not be attributed to nuclear uncertainties, and points to issues in massive-star models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.01723v1-abstract-full').style.display = 'none'; document.getElementById('2412.01723v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Communications ( 2024) 15:9608 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.03664">arXiv:2101.03664</a> <span> [<a href="https://arxiv.org/pdf/2101.03664">pdf</a>, <a href="https://arxiv.org/format/2101.03664">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.125.262701">10.1103/PhysRevLett.125.262701 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> $尾$-decay of $^{61}$V and its Role in Cooling Accreted Neutron Star Crusts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ong%2C+W+-">W. -J. Ong</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+E+F">E. F. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Browne%2C+J">J. Browne</a>, <a href="/search/nucl-ex?searchtype=author&query=Ahn%2C+S">S. Ahn</a>, <a href="/search/nucl-ex?searchtype=author&query=Childers%2C+K">K. Childers</a>, <a href="/search/nucl-ex?searchtype=author&query=Crider%2C+B+P">B. P. Crider</a>, <a href="/search/nucl-ex?searchtype=author&query=Dombos%2C+A+C">A. C. Dombos</a>, <a href="/search/nucl-ex?searchtype=author&query=Gupta%2C+S+S">S. S. Gupta</a>, <a href="/search/nucl-ex?searchtype=author&query=Hitt%2C+G+W">G. W. Hitt</a>, <a href="/search/nucl-ex?searchtype=author&query=Langer%2C+C">C. Langer</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Liddick%2C+S+N">S. N. Liddick</a>, <a href="/search/nucl-ex?searchtype=author&query=Lyons%2C+S">S. Lyons</a>, <a href="/search/nucl-ex?searchtype=author&query=Meisel%2C+Z">Z. Meisel</a>, <a href="/search/nucl-ex?searchtype=author&query=M%C3%B6ller%2C+P">P. M枚ller</a>, <a href="/search/nucl-ex?searchtype=author&query=Montes%2C+F">F. Montes</a>, <a href="/search/nucl-ex?searchtype=author&query=Naqvi%2C+F">F. Naqvi</a>, <a href="/search/nucl-ex?searchtype=author&query=Pereira%2C+J">J. Pereira</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokop%2C+C">C. Prokop</a>, <a href="/search/nucl-ex?searchtype=author&query=Richman%2C+D">D. Richman</a>, <a href="/search/nucl-ex?searchtype=author&query=Schatz%2C+H">H. Schatz</a>, <a href="/search/nucl-ex?searchtype=author&query=Schmidt%2C+K">K. Schmidt</a>, <a href="/search/nucl-ex?searchtype=author&query=Spyrou%2C+A">A. Spyrou</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="2101.03664v1-abstract-short" style="display: inline;"> The interpretation of observations of cooling neutron star crusts in quasi-persistent X-ray transients is affected by predictions of the strength of neutrino cooling via crust Urca processes. The strength of crust Urca neutrino cooling depends sensitively on the electron-capture and $尾$-decay ground-state to ground-state transition strengths of neutron-rich rare isotopes. Nuclei with mass number… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03664v1-abstract-full').style.display = 'inline'; document.getElementById('2101.03664v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03664v1-abstract-full" style="display: none;"> The interpretation of observations of cooling neutron star crusts in quasi-persistent X-ray transients is affected by predictions of the strength of neutrino cooling via crust Urca processes. The strength of crust Urca neutrino cooling depends sensitively on the electron-capture and $尾$-decay ground-state to ground-state transition strengths of neutron-rich rare isotopes. Nuclei with mass number $A=61$ are predicted to be among the most abundant in accreted crusts, and the last remaining experimentally undetermined ground-state to ground-state transition strength was the $尾$-decay of $^{61}$V. This work reports the first experimental determination of this transition strength, a ground-state branching of 8.1$^{+2.2}_{-2.0} \%$, corresponding to a log $ft$ value of 5.5$^{+0.2}_{-0.2}$. This result was achieved through the measurement of the $尾$-delayed $纬$ rays using the total absorption spectrometer SuN and the measurement of the $尾$-delayed neutron branch using the neutron long counter system NERO at the National Superconducting Cyclotron Laboratory at Michigan State University. This method helps to mitigate the impact of the Pandemonium effect in extremely neutron-rich nuclei on experimental results. The result implies that $A=61$ nuclei do not provide the strongest cooling in accreted neutron star crusts as expected by some predictions, but that their cooling is still larger compared to most other mass numbers. Only nuclei with mass numbers 31, 33, and 55 are predicted to be cooling more strongly. However, the theoretical predictions for the transition strengths of these nuclei are not consistently accurate enough to draw conclusions on crust cooling. With the experimental approach developed in this work all relevant transitions are within reach to be studied in the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03664v1-abstract-full').style.display = 'none'; document.getElementById('2101.03664v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">6 pages, 3 figures Copyright by APS Link to publication: https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.125.262701</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 125 (2020) 262701 published December 28, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1805.00856">arXiv:1805.00856</a> <span> [<a href="https://arxiv.org/pdf/1805.00856">pdf</a>, <a href="https://arxiv.org/format/1805.00856">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.97.054329">10.1103/PhysRevC.97.054329 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enhanced low-energy $纬$-decay strength of $^{70}$Ni and its robustness within the shell model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Larsen%2C+A+C">A. C. Larsen</a>, <a href="/search/nucl-ex?searchtype=author&query=Midtb%C3%B8%2C+J+E">J. E. Midtb酶</a>, <a href="/search/nucl-ex?searchtype=author&query=Guttormsen%2C+M">M. Guttormsen</a>, <a href="/search/nucl-ex?searchtype=author&query=Renstr%C3%B8m%2C+T">T. Renstr酶m</a>, <a href="/search/nucl-ex?searchtype=author&query=Liddick%2C+S+N">S. N. Liddick</a>, <a href="/search/nucl-ex?searchtype=author&query=Spyrou%2C+A">A. Spyrou</a>, <a href="/search/nucl-ex?searchtype=author&query=Karampagia%2C+S">S. Karampagia</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Achakovskiy%2C+O">O. Achakovskiy</a>, <a href="/search/nucl-ex?searchtype=author&query=Kamerdzhiev%2C+S">S. Kamerdzhiev</a>, <a href="/search/nucl-ex?searchtype=author&query=Bleuel%2C+D+L">D. L. Bleuel</a>, <a href="/search/nucl-ex?searchtype=author&query=Couture%2C+A">A. Couture</a>, <a href="/search/nucl-ex?searchtype=author&query=Campo%2C+L+C">L. Crespo Campo</a>, <a href="/search/nucl-ex?searchtype=author&query=Crider%2C+B+P">B. P. Crider</a>, <a href="/search/nucl-ex?searchtype=author&query=Dombos%2C+A+C">A. C. Dombos</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Mosby%2C+S">S. Mosby</a>, <a href="/search/nucl-ex?searchtype=author&query=Naqvi%2C+F">F. Naqvi</a>, <a href="/search/nucl-ex?searchtype=author&query=Perdikakis%2C+G">G. Perdikakis</a>, <a href="/search/nucl-ex?searchtype=author&query=Prokop%2C+C+J">C. J. Prokop</a>, <a href="/search/nucl-ex?searchtype=author&query=Quinn%2C+S+J">S. J. Quinn</a>, <a href="/search/nucl-ex?searchtype=author&query=Siem%2C+S">S. Siem</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="1805.00856v2-abstract-short" style="display: inline;"> Neutron-capture reactions on very neutron-rich nuclei are essential for heavy-element nucleosynthesis through the rapid neutron-capture process, now shown to take place in neutron-star merger events. For these exotic nuclei, radiative neutron capture is extremely sensitive to their $纬$-emission probability at very low $纬$ energies. In this work, we present measurements of the $纬$-decay strength of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.00856v2-abstract-full').style.display = 'inline'; document.getElementById('1805.00856v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1805.00856v2-abstract-full" style="display: none;"> Neutron-capture reactions on very neutron-rich nuclei are essential for heavy-element nucleosynthesis through the rapid neutron-capture process, now shown to take place in neutron-star merger events. For these exotic nuclei, radiative neutron capture is extremely sensitive to their $纬$-emission probability at very low $纬$ energies. In this work, we present measurements of the $纬$-decay strength of $^{70}$Ni over the wide range $1.3 \leq E_纬 \leq 8 $ MeV. A significant enhancement is found in the $纬$-decay strength for transitions with $E_纬< 3$ MeV. At present, this is the most neutron-rich nucleus displaying this feature, proving that this phenomenon is not restricted to stable nuclei. We have performed $E1$-strength calculations within the quasiparticle time-blocking approximation, which describe our data above $E_纬\simeq 5$ MeV very well. Moreover, large-scale shell-model calculations indicate an $M1$ nature of the low-energy $纬$ strength. This turns out to be remarkably robust with respect to the choice of interaction, truncation and model space, and we predict its presence in the whole isotopic chain, in particular the neutron-rich $^{72,74,76}\mathrm{Ni}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1805.00856v2-abstract-full').style.display = 'none'; document.getElementById('1805.00856v2-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> 22 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 May, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">9 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 97, 054329 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-th/0703051">arXiv:nucl-th/0703051</a> <span> [<a href="https://arxiv.org/pdf/nucl-th/0703051">pdf</a>, <a href="https://arxiv.org/ps/nucl-th/0703051">ps</a>, <a href="https://arxiv.org/format/nucl-th/0703051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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.99.072001">10.1103/PhysRevLett.99.072001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Isospin mixing in the nucleon and 4He and the nucleon strange electric form factor </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Viviani%2C+M">M. Viviani</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiavilla%2C+R">R. Schiavilla</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubis%2C+B">B. Kubis</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Girlanda%2C+L">L. Girlanda</a>, <a href="/search/nucl-ex?searchtype=author&query=Kievsky%2C+A">A. Kievsky</a>, <a href="/search/nucl-ex?searchtype=author&query=Marcucci%2C+L+E">L. E. Marcucci</a>, <a href="/search/nucl-ex?searchtype=author&query=Rosati%2C+S">S. Rosati</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="nucl-th/0703051v1-abstract-short" style="display: inline;"> In order to isolate the contribution of the nucleon strange electric form factor to the parity-violating asymmetry measured in 4He(\vec e,e')4He experiments, it is crucial to have a reliable estimate of the magnitude of isospin-symmetry-breaking (ISB) corrections in both the nucleon and 4He. We examine this issue in the present letter. Isospin admixtures in the nucleon are determined in chiral p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0703051v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-th/0703051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-th/0703051v1-abstract-full" style="display: none;"> In order to isolate the contribution of the nucleon strange electric form factor to the parity-violating asymmetry measured in 4He(\vec e,e')4He experiments, it is crucial to have a reliable estimate of the magnitude of isospin-symmetry-breaking (ISB) corrections in both the nucleon and 4He. We examine this issue in the present letter. Isospin admixtures in the nucleon are determined in chiral perturbation theory, while those in 4He are derived from nuclear interactions, including explicit ISB terms. A careful analysis of the model dependence in the resulting predictions for the nucleon and nuclear ISB contributions to the asymmetry is carried out. We conclude that, at the low momentum transfers of interest in recent measurements reported by the HAPPEX collaboration at Jefferson Lab, these contributions are of comparable magnitude to those associated with strangeness components in the nucleon electric form factor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0703051v1-abstract-full').style.display = 'none'; document.getElementById('nucl-th/0703051v1-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 March, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2007. </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, 2 figures, revtex4</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> HISKP-TH-07/08 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.99:112002,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-th/0608079">arXiv:nucl-th/0608079</a> <span> [<a href="https://arxiv.org/pdf/nucl-th/0608079">pdf</a>, <a href="https://arxiv.org/ps/nucl-th/0608079">ps</a>, <a href="https://arxiv.org/format/nucl-th/0608079">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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 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/i2006-10401-5">10.1140/epja/i2006-10401-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Isospin breaking in the vector current of the nucleon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">Randy Lewis</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="nucl-th/0608079v2-abstract-short" style="display: inline;"> Extraction of the nucleon's strange form factors from experimental data requires a quantitative understanding of the unavoidable contamination from isospin violation. A number of authors have addressed this issue during the past decade, and their work is reviewed here. The predictions from early models are largely consistent with recent results that rely as much as possible on input from QCD sym… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0608079v2-abstract-full').style.display = 'inline'; document.getElementById('nucl-th/0608079v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-th/0608079v2-abstract-full" style="display: none;"> Extraction of the nucleon's strange form factors from experimental data requires a quantitative understanding of the unavoidable contamination from isospin violation. A number of authors have addressed this issue during the past decade, and their work is reviewed here. The predictions from early models are largely consistent with recent results that rely as much as possible on input from QCD symmetries and related experimental data. The resulting bounds on isospin violation are sufficiently precise to be of value to on-going experimental and theoretical studies of the nucleon's strange form factors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0608079v2-abstract-full').style.display = 'none'; document.getElementById('nucl-th/0608079v2-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, 2006; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 August, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2006. </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. Presented at the International Workshop "From Parity Violation to Hadronic Structure and more...", Milos, Greece, 16-20 May 2006. Version 2 is only to update Refs. [21] and [25]</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur.Phys.J.A32:409-414,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-th/0605006">arXiv:nucl-th/0605006</a> <span> [<a href="https://arxiv.org/pdf/nucl-th/0605006">pdf</a>, <a href="https://arxiv.org/ps/nucl-th/0605006">ps</a>, <a href="https://arxiv.org/format/nucl-th/0605006">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</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 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.74.015204">10.1103/PhysRevC.74.015204 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Isospin violation in the vector form factors of the nucleon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Kubis%2C+B">Bastian Kubis</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">Randy Lewis</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="nucl-th/0605006v1-abstract-short" style="display: inline;"> A quantitative understanding of isospin violation is an increasingly important ingredient for the extraction of the nucleon's strange vector form factors from experimental data. We calculate the isospin violating electric and magnetic form factors in chiral perturbation theory to leading and next-to-leading order respectively, and we extract the low-energy constants from resonance saturation. Un… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0605006v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-th/0605006v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-th/0605006v1-abstract-full" style="display: none;"> A quantitative understanding of isospin violation is an increasingly important ingredient for the extraction of the nucleon's strange vector form factors from experimental data. We calculate the isospin violating electric and magnetic form factors in chiral perturbation theory to leading and next-to-leading order respectively, and we extract the low-energy constants from resonance saturation. Uncertainties are dominated largely by limitations in the current knowledge of some vector meson couplings. The resulting bounds on isospin violation are sufficiently precise to be of value to on-going experimental studies of the strange form factors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-th/0605006v1-abstract-full').style.display = 'none'; document.getElementById('nucl-th/0605006v1-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 May, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2006. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures, uses RevTeX</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> HISKP-TH-06/10 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C74:015204,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-lat/0409081">arXiv:hep-lat/0409081</a> <span> [<a href="https://arxiv.org/pdf/hep-lat/0409081">pdf</a>, <a href="https://arxiv.org/ps/hep-lat/0409081">ps</a>, <a href="https://arxiv.org/format/hep-lat/0409081">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 - Lattice">hep-lat</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/10.1016/j.nuclphysbps.2004.11.333">10.1016/j.nuclphysbps.2004.11.333 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pion form factor using domain wall valence and asqtad sea quarks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=LHP+Collaboration"> LHP Collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Fleming%2C+G+T">George T. Fleming</a>, <a href="/search/nucl-ex?searchtype=author&query=Bonnet%2C+F+D+R">Frederic D. R. Bonnet</a>, <a href="/search/nucl-ex?searchtype=author&query=Edwards%2C+R+G">Robert G. Edwards</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">Randy Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Richards%2C+D+G">David G. Richards</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="hep-lat/0409081v1-abstract-short" style="display: inline;"> We compute the pion electromagnetic form factor in a hybrid calculation with domain wall valence quarks and improved staggered (asqtad) sea quarks. This method can easily be extended to rho-to-gamma-pi transition form factors. </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-lat/0409081v1-abstract-full" style="display: none;"> We compute the pion electromagnetic form factor in a hybrid calculation with domain wall valence quarks and improved staggered (asqtad) sea quarks. This method can easily be extended to rho-to-gamma-pi transition form factors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-lat/0409081v1-abstract-full').style.display = 'none'; document.getElementById('hep-lat/0409081v1-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 September, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">3 pages, 3 figures, Lattice2004(spectrum)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys.Proc.Suppl.140:302-304,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0308008">arXiv:nucl-ex/0308008</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0308008">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0308008">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0308008">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.69.048801">10.1103/PhysRevC.69.048801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Particle decay branching ratios for states of astrophysical importance in 19Ne </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Visser%2C+D+W">D. W. Visser</a>, <a href="/search/nucl-ex?searchtype=author&query=Caggiano%2C+J+A">J. A. Caggiano</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Handler%2C+W+B">W. B. Handler</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</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="nucl-ex/0308008v3-abstract-short" style="display: inline;"> We have measured proton and alpha-particle branching ratios of excited states in 19Ne formed using the 19F(3He,t) reaction at a beam energy of 25 MeV. These ratios have a large impact on the astrophysical reaction rates of 15O(alpha,gamma), 18F(p,gamma) and 18F(p,alpha), which are of interest in understanding energy generation in x-ray bursts and in interpreting anticipated gamma-ray observation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308008v3-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0308008v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0308008v3-abstract-full" style="display: none;"> We have measured proton and alpha-particle branching ratios of excited states in 19Ne formed using the 19F(3He,t) reaction at a beam energy of 25 MeV. These ratios have a large impact on the astrophysical reaction rates of 15O(alpha,gamma), 18F(p,gamma) and 18F(p,alpha), which are of interest in understanding energy generation in x-ray bursts and in interpreting anticipated gamma-ray observations of novae. We detect decay protons and alpha-particles using a silicon detector array in coincidence with tritons measured in the focal plane detector of our Enge split-pole spectrograph. The silicon array consists of five strip detectors of the type used in the Louvain-Edinburgh Detector Array, subtending angles from 130 degrees to 165 degrees with approximately 14% lab efficiency. The correlation angular distributions give additional confidence in some prior spin-parity assignments that were based on gamma branchings. We measure Gamma_p/Gamma=0.387+-0.016 for the 665 keV proton resonance, which agrees well with the direct measurement of Bardayan et al. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308008v3-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0308008v3-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 February, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 August, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2003. </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, 2 figures, 3 tables. Prepared using RevTex 4 and BibTex. Further minor revisions, incl. fig. 1 font size increase, 1 table removal, and minor changes to the text</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev. C69 (2004) 048801 </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/0303285">arXiv:astro-ph/0303285</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0303285">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0303285">ps</a>, <a href="https://arxiv.org/format/astro-ph/0303285">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="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.90.162501">10.1103/PhysRevLett.90.162501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 21Na(p,gamma)22Mg Reaction and Oxygen-Neon Novae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Bishop%2C+S">S. Bishop</a>, <a href="/search/nucl-ex?searchtype=author&query=Azuma%2C+R+E">R. E. Azuma</a>, <a href="/search/nucl-ex?searchtype=author&query=Buchmann%2C+L">L. Buchmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Chatterjee%2C+M+L">M. L. Chatterjee</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Auria%2C+J+M">J. M. D'Auria</a>, <a href="/search/nucl-ex?searchtype=author&query=Engel%2C+S">S. Engel</a>, <a href="/search/nucl-ex?searchtype=author&query=Gigliotti%2C+D">D. Gigliotti</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U. Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/nucl-ex?searchtype=author&query=Hunter%2C+D">D. Hunter</a>, <a href="/search/nucl-ex?searchtype=author&query=Hussein%2C+A">A. Hussein</a>, <a href="/search/nucl-ex?searchtype=author&query=Hutcheon%2C+D">D. Hutcheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Jewett%2C+C">C. Jewett</a>, <a href="/search/nucl-ex?searchtype=author&query=Jose%2C+J">J. Jose</a>, <a href="/search/nucl-ex?searchtype=author&query=King%2C+J">J. King</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Lamey%2C+M">M. Lamey</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Liu%2C+W">W. Liu</a>, <a href="/search/nucl-ex?searchtype=author&query=Michimasa%2C+S">S. Michimasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Olin%2C+A">A. Olin</a>, <a href="/search/nucl-ex?searchtype=author&query=Ottewell%2C+D">D. Ottewell</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</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="astro-ph/0303285v1-abstract-short" style="display: inline;"> The 21Na(p,gamma)22Mg reaction is expected to play an important role in the nucleosynthesis of 22Na in Oxygen-Neon novae. The decay of 22Na leads to the emission of a characteristic 1.275 MeV gamma-ray line. This report provides the first direct measurement of the rate of this reaction using a radioactive 21Na beam, and discusses its astrophysical implications. The energy of the important state… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0303285v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0303285v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0303285v1-abstract-full" style="display: none;"> The 21Na(p,gamma)22Mg reaction is expected to play an important role in the nucleosynthesis of 22Na in Oxygen-Neon novae. The decay of 22Na leads to the emission of a characteristic 1.275 MeV gamma-ray line. This report provides the first direct measurement of the rate of this reaction using a radioactive 21Na beam, and discusses its astrophysical implications. The energy of the important state was measured to be E$_{c.m.}$= 205.7 $\pm$ 0.5 keV with a resonance strength $蠅纬= 1.03\pm0.16_{stat}\pm0.14_{sys}$ meV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0303285v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0303285v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 March, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2003. </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 Physical Review Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.90:162501,2003; Erratum-ibid.90:229902,2003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/9706004">arXiv:nucl-ex/9706004</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/9706004">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/9706004">ps</a>, <a href="https://arxiv.org/format/nucl-ex/9706004">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/PhysRevLett.79.3612">10.1103/PhysRevLett.79.3612 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Charged Strange Quark Matter Produced in 11.5 A GeV/c Au + Pb Collisions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=E864+Collaboration"> E864 Collaboration</a>, <a href="/search/nucl-ex?searchtype=author&query=Armstrong%2C+T+A">T. A. Armstrong</a>, <a href="/search/nucl-ex?searchtype=author&query=Barish%2C+K+N">K. N. Barish</a>, <a href="/search/nucl-ex?searchtype=author&query=Bennett%2C+S+J">S. J. Bennett</a>, <a href="/search/nucl-ex?searchtype=author&query=Chikanian%2C+A">A. Chikanian</a>, <a href="/search/nucl-ex?searchtype=author&query=Coe%2C+S+D">S. D. Coe</a>, <a href="/search/nucl-ex?searchtype=author&query=Cormier%2C+T+M">T. M. Cormier</a>, <a href="/search/nucl-ex?searchtype=author&query=Davies%2C+R">R. Davies</a>, <a href="/search/nucl-ex?searchtype=author&query=DeCataldo%2C+G">G. DeCataldo</a>, <a href="/search/nucl-ex?searchtype=author&query=Dee%2C+P">P. Dee</a>, <a href="/search/nucl-ex?searchtype=author&query=Diebold%2C+G+E">G. E. Diebold</a>, <a href="/search/nucl-ex?searchtype=author&query=Dover%2C+C+B">C. B. Dover</a>, <a href="/search/nucl-ex?searchtype=author&query=Fachini%2C+P">P. Fachini</a>, <a href="/search/nucl-ex?searchtype=author&query=Finch%2C+L+E">L. E. Finch</a>, <a href="/search/nucl-ex?searchtype=author&query=George%2C+N+K">N. K. George</a>, <a href="/search/nucl-ex?searchtype=author&query=Giglietto%2C+N">N. Giglietto</a>, <a href="/search/nucl-ex?searchtype=author&query=Greene%2C+S+V">S. V. Greene</a>, <a href="/search/nucl-ex?searchtype=author&query=Haridas%2C+P">P. Haridas</a>, <a href="/search/nucl-ex?searchtype=author&query=Hill%2C+J+C">J. C. Hill</a>, <a href="/search/nucl-ex?searchtype=author&query=Hirsch%2C+A+S">A. S. Hirsch</a>, <a href="/search/nucl-ex?searchtype=author&query=Hoversten%2C+R+A">R. A. Hoversten</a>, <a href="/search/nucl-ex?searchtype=author&query=Huang%2C+H+Z">H. Z. Huang</a>, <a href="/search/nucl-ex?searchtype=author&query=Kim%2C+B">B. Kim</a>, <a href="/search/nucl-ex?searchtype=author&query=Kumar%2C+B+S">B. S. Kumar</a>, <a href="/search/nucl-ex?searchtype=author&query=Lainis%2C+T">T. Lainis</a> , et al. (30 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="nucl-ex/9706004v1-abstract-short" style="display: inline;"> We present results of a search for strange quark matter (strangelets) in 11.5 A GeV/c Au+Pb collisions from the 1994 and 1995 runs of experiment E864 at Brookhaven's AGS. We observe no strangelet candidates and set a 90% confidence level upper limit of approximately 3x10**-8 per 10% central interaction for the production of |Z|=1 and |Z|=2 strangelets over a large mass range and with metastable… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/9706004v1-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/9706004v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/9706004v1-abstract-full" style="display: none;"> We present results of a search for strange quark matter (strangelets) in 11.5 A GeV/c Au+Pb collisions from the 1994 and 1995 runs of experiment E864 at Brookhaven's AGS. We observe no strangelet candidates and set a 90% confidence level upper limit of approximately 3x10**-8 per 10% central interaction for the production of |Z|=1 and |Z|=2 strangelets over a large mass range and with metastable lifetimes of about 50 ns or more. These results place constraints primarily on quark-gluon plasma based production models for strangelets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/9706004v1-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/9706004v1-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 June, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1997. </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, 3 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.79:3612-3616,1997 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ex/9506015">arXiv:hep-ex/9506015</a> <span> [<a href="https://arxiv.org/pdf/hep-ex/9506015">pdf</a>, <a href="https://arxiv.org/ps/hep-ex/9506015">ps</a>, <a href="https://arxiv.org/format/hep-ex/9506015">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/10.1016/0375-9601(96)00189-2">10.1016/0375-9601(96)00189-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Are Antiprotons Forever? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Holzscheiter%2C+M+H">M. H. Holzscheiter</a>, <a href="/search/nucl-ex?searchtype=author&query=Feng%2C+X">X. Feng</a>, <a href="/search/nucl-ex?searchtype=author&query=Goldman%2C+T">T. Goldman</a>, <a href="/search/nucl-ex?searchtype=author&query=King%2C+N+S+P">N. S. P. King</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R+A">R. A. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Nieto%2C+M+M">M. M. Nieto</a>, <a href="/search/nucl-ex?searchtype=author&query=Smith%2C+G+A">G. A. Smith</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="hep-ex/9506015v3-abstract-short" style="display: inline;"> Up to one million antiprotons from a single LEAR spill have been captured in a large Penning trap. Surprisingly, when the antiprotons are cooled to energies significantly below 1 eV, the annihilation rate falls below background. Thus, very long storage times for antiprotons have been demonstrated in the trap, even at the compromised vacuum conditions imposed by the experimental set up. The signi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/9506015v3-abstract-full').style.display = 'inline'; document.getElementById('hep-ex/9506015v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ex/9506015v3-abstract-full" style="display: none;"> Up to one million antiprotons from a single LEAR spill have been captured in a large Penning trap. Surprisingly, when the antiprotons are cooled to energies significantly below 1 eV, the annihilation rate falls below background. Thus, very long storage times for antiprotons have been demonstrated in the trap, even at the compromised vacuum conditions imposed by the experimental set up. The significance for future ultra-low energy experiments, including portable antiproton traps, is discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ex/9506015v3-abstract-full').style.display = 'none'; document.getElementById('hep-ex/9506015v3-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 October, 1995; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 June, 1995; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 1995. </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, latex; 4 figures, uufiled. Slightly expanded discussion of expected energy dependence of annihilation cross section and rate, and of estimates of trap pressure, plus minor text improvements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LA-UR-95-1604 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.A214:279,1996 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul 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