Comparison of the Core-collapse Evolution of Two Nearly Equal-mass Progenitors

Bruenn, Stephen W.; Sieverding, Andre; Lentz, Eric J.; Sukhbold, Tuguldur; Hix, W. Raphael; Huk, Leah N.; Harris, J. Austin; Messer, O. E. Bronson; Mezzacappa, Anthony

doi:10.3847/1538-4357/acbb65

Title: Comparison of the Core-collapse Evolution of Two Nearly Equal-mass Progenitors

Journal Article · Tue Apr 18 00:00:00 EDT 2023 · The Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/acbb65· OSTI ID:1970397

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Abstract We compare the core-collapse evolution of a pair of 15.8 M _☉ stars with significantly different internal structures, a consequence of the bimodal variability exhibited by massive stars during their late evolutionary stages. The 15.78 and 15.79 M _☉ progenitors have core masses (masses interior to an entropy of 4 k _B baryon ⁻¹ ) of 1.47 and 1.78 M _☉ and compactness parameters ξ _1.75 of 0.302 and 0.604, respectively. The core-collapse simulations are carried out in 2D to nearly 3 s postbounce and show substantial differences in the times of shock revival and explosion energies. The 15.78 M _☉ model begins exploding promptly at 120 ms postbounce when a strong density decrement at the Si–Si/O shell interface, not present in the 15.79 M _☉ progenitor, encounters the stalled shock. The 15.79 M _☉ model takes 100 ms longer to explode but ultimately produces a more powerful explosion. Both the larger mass accretion rate and the more massive core of the 15.79 M _☉ model during the first 0.8 s postbounce time result in larger ν _e / ${\bar{ν}}_{e}$ luminosities and RMS energies along with a flatter and higher-density heating region. The more-energetic explosion of the 15.79 M _☉ model resulted in the ejection of twice as much ⁵⁶ Ni. Most of the ejecta in both models are moderately proton rich, though counterintuitively the highest electron fraction ( Y _e = 0.61) ejecta in either model are in the less-energetic 15.78 M _☉ model, while the lowest electron fraction ( Y _e = 0.45) ejecta in either model are in the 15.79 M _☉ model.

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Research Organization:: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)

Sponsoring Organization:: USDOE Office of Science (SC), Nuclear Physics (NP); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR); National Aeronautics and Space Administration (NASA); National Science Foundation (NSF)

Grant/Contract Number:: AC05-00OR22725; AC02-05CH11231; NNH11AQ72I; OCI-0749242; OCI-0749204; OCI-0749248; PHY-1913531; PHY-1516197; AST-0653376

OSTI ID:: 1970397

Alternate ID(s):: OSTI ID: 1971043

Journal Information:: The Astrophysical Journal, Journal Name: The Astrophysical Journal Vol. 947 Journal Issue: 1; ISSN 0004-637X

Publisher:: American Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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