Bulletin of the American Physical Society
6th Joint Meeting of the APS Division of Nuclear Physics and the Physical Society of Japan
Sunday–Friday, November 26–December 1 2023; Hawaii, the Big Island
Session M09: Nuclear Astrophysics VI |
Hide Abstracts |
Chair: Erin Good, FRIB Room: Hilton Waikoloa Village Kohala 2 |
Friday, December 1, 2023 2:00PM - 2:15PM |
M09.00001: Core-collapse supernovae and neutrino oscillation Tomoya Takiwaki After intensive and extensive basic research, it is gradually known that neutrino oscillations affect the dynamics of supernova explosions. Since the density of neutrino gas is so high near neutron stars, neutrino self-interaction that induced by scattering of neutrino, are particularly important. Among them, so-called fast flavor oscillation or collisional instability may become a game changer. In this talk, we report recent progress on the supernova simulations and results of systematic study of neutrino oscillation. |
Friday, December 1, 2023 2:15PM - 2:30PM |
M09.00002: Large scale tabulated neutrino opacity table for next-generation simulations of core-collapse supernovae/binary neutron star mergers Zidu Lin, Andrew Steiner, Jerome Margueron, Gianluca Colo The neutrino opacities of hot and dense matter play an important role in the core collapse supernovae (CCSNe) explosion mechanism, the nucleosynthesis process in CCSNe and binary neutron star (BNS) mergers, and the fast neutrino flavor conversions. The neutrino-nucleon interactions are one of the main sources of neutrino opacities. An accrate discription of massive star neutrino opacities requires one to take into account both the many-body corrections in dense matter and the kinematics constraints of neutrino-nucleon reactions in an extremely wide range of densities, temperatures, proton fractions and incoming neutrino energies. This has not been fully achieved in the state-of-the-art numerical simulations of CCSNe and BNS merger. In this talk, I would like to introduce our work on constructing large scale tabulated neutrino opacity table for next-generation simulations of core-collapse supernovae/binary neutron star mergers, which applies random phase approximations that consistent with underlying equation of states to estimate the many-body corrections on neutrino-nucleon opacities. I will also discuss the uncertainties and the possible experimental constraints for neutrino opacities in different regions (densities, temperatures, proton fractions) of our table. |
Friday, December 1, 2023 2:30PM - 2:45PM |
M09.00003: Status of cosmic antinuclei searches Philip von Doetinchem The precise measurement of cosmic antinuclei serves as important means for identifying the nature of dark matter and other beyond-standard-model physics. Recent years showed that identifying the nature of dark matter with cosmic positrons and antiprotons is difficult, and has lead to a significantly increased interest in cosmic antideuteron and antihelium searches. Antideuterons and antihelium nuclei may also be generated in dark matter annihilations or decays, offering a potential breakthrough in unexplored phase space for dark matter. This presentation discusses the current status, perspectives, and challenges for cosmic antinuclei searches. It will review the motivation for antinuclei searches, discuss the theoretical and experimental uncertainties of antinuclei production and propagation in our Galaxy, as well as summarize the experimental status. |
Friday, December 1, 2023 2:45PM - 3:00PM Withdrawn |
M09.00004: Strength measurement of the 830 keV resonance in 22Ne(α,n)25Mg reaction using a stilbene detector Shahina Shahina, Richard J deBoer, Joachim Gorres, Michael T Febbraro, Rebeka Kelmar, Miriam Matney, Khachatur Manukyan, Jason Nattress, Edward Stech, Michael C F Wiescher The interplay and correlation between the 22Ne(α,γ)26Mg and the competing 22Ne(α,n)25Mg reaction determines the efficiency of the latter as a neutron source in stellar helium burning. In both cases, the reaction rates are dominated by the strength of the α-cluster resonance at 830 keV. This resonance plays a particularly important role in determining the strength of the neutron flux for weak and main s-process as well as n-process environments. Recent experimental studies based on transfer reactions suggest that the neutron and γ-ray strengths are approximately equal. In this new and independent study performed at Notre Dame using a stilbene detector, the 22Ne(α,n)25Mg resonance strength is remeasured and found to be similar to the previous direct study. This reinforces an 830 keV resonance strength that is approximately a factor of three larger for the 22Ne(α,n)25Mg reaction than for the 22Ne(α,γ)26Mg reaction. |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700