Finite-temperature electron-capture rates for neutron-rich nuclei around N=50 and effects on core-collapse supernovae simulations

التفاصيل البيبلوغرافية
العنوان: Finite-temperature electron-capture rates for neutron-rich nuclei around N=50 and effects on core-collapse supernovae simulations
المؤلفون: Giraud, S., Ney, E. M., Ravlić, A., Zegers, R. G. T., Engel, J., Paar, N., Brown, B. A., Gabler, J. -M., Lesniak, J., Rebenstock, J.
سنة النشر: 2021
المجموعة: Astrophysics
Nuclear Theory
مصطلحات موضوعية: Nuclear Theory, Astrophysics - Solar and Stellar Astrophysics
الوصف: The temperature dependence of stellar electron-capture (EC) rates is investigated, with a focus on nuclei around $N=50$, just above $Z=28$, which play an important role during the collapse phase of core-collapse supernovae (CCSN). Two new microscopic calculations of stellar EC rates are obtained from a relativistic and a non-relativistic finite-temperature quasiparticle random-phase approximation approaches, for a conventional grid of temperatures and densities. In both approaches, EC rates due to Gamow-Teller transitions are included. In the relativistic calculation contributions from first-forbidden transitions are also included, and add strongly to the EC rates. The new EC rates are compared with large-scale shell model calculations for the specific case of $^{86}$Kr, providing insight into the finite-temperature effects on the EC rates. At relevant thermodynamic conditions for core-collapse, the discrepancies between the different calculations of this work are within about one order of magnitude. Numerical simulations of CCSN are performed with the spherically-symmetric GR1D simulation code to quantify the impact of such differences on the dynamics of the collapse. These simulations also include EC rates based on two parametrized approximations. A comparison of the neutrino luminosities and enclosed mass at core bounce shows that differences between simulations with different sets of EC rates are relatively small ($\approx 5\%$), suggesting that the EC rates used as inputs for these simulations have become well constrained.
نوع الوثيقة: Working Paper
DOI: 10.1103/PhysRevC.105.055801
URL الوصول: http://arxiv.org/abs/2112.01626
رقم الأكسشن: edsarx.2112.01626
قاعدة البيانات: arXiv
الوصف
DOI:10.1103/PhysRevC.105.055801