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

Giraud, S.; Zegers, R. T.; Brown, B. A.; Gabler, J. -M.; Lesniak, J.; Rebenstock, J.; Ney, E. M.; Engel, J.; Ravlić, A.; Paar, N.

doi:10.1103/physrevc.105.055801

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

Journal Article · Wed May 04 00:00:00 EDT 2022 · Physical Review. C

DOI:https://doi.org/10.1103/physrevc.105.055801· OSTI ID:1979881

^[1]; Zegers, R. T. ^[2]; Brown, B. A. ^[2]; Gabler, J. -M. ^[2]; Lesniak, J. ^[2]; Rebenstock, J. ^[2]; ^[3]; Engel, J. ^[3]; Ravlić, A. ^[4]; Paar, N. ^[4]

Michigan State University, East Lansing, MI (United States); OSTI
Michigan State University, East Lansing, MI (United States)
University of North Carolina, Chapel Hill, NC (United States). Dept. of Chemistry
University of Zagreb (Croatia)

In this paper the temperature dependence of stellar electron-capture (EC) rates is investigated, with a focus on nuclei near 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 relativistic and nonrelativistic 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 ⁸⁶Kr, 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 paper 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 (≈ 5 %), suggesting that the EC rates used as inputs for these simulations have become well constrained.

View Accepted Manuscript (DOE)

Research Organization:: Michigan State University, East Lansing, MI (United States); University of Tennessee, Knoxville, TN (United States)

Sponsoring Organization:: European Union; National Science Foundation (NSF); QuantiXLie Centre of Excellence; USDOE Office of Science (SC)

Grant/Contract Number:: SC0018223

OSTI ID:: 1979881

Journal Information:: Physical Review. C, Journal Name: Physical Review. C Journal Issue: 5 Vol. 105; ISSN 2469-9985

Publisher:: American Physical Society (APS)Copyright Statement

Country of Publication:: United States

Language:: English

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