Equation-of-state Dependence of Gravitational Waves in Core-collapse Supernovae

Eggenberger Andersen, Oliver; Zha, Shuai; da Silva Schneider, André; Betranhandy, Aurore; Couch, Sean M.; O’Connor, Evan P.

doi:10.3847/1538-4357/ac294c

Title: Equation-of-state Dependence of Gravitational Waves in Core-collapse Supernovae

Journal Article · Wed Dec 22 00:00:00 EST 2021 · The Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/ac294c· OSTI ID:1981233

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Stockholm Univ. (Sweden)
Michigan State Univ., East Lansing, MI (United States)

Gravitational waves (GWs) provide unobscured insight into the birthplace of neutron stars and black holes in core-collapse supernovae (CCSNe). The nuclear equation of state (EOS) describing these dense environments is yet uncertain, and variations in its prescription affect the proto-neutron star (PNS) and the post-bounce dynamics in CCSN simulations, subsequently impacting the GW emission. In this study, we perform axisymmetric simulations of CCSNe with Skyrme-type EOSs to study how the GW signal and PNS convection zone are impacted by two experimentally accessible EOS parameters, (1) the effective mass of nucleons, m*, which is crucial in setting the thermal dependence of the EOS, and (2) the isoscalar incompressibility modulus, K_sat. While K_sat shows little impact, the peak frequency of the GWs has a strong effective mass dependence due to faster contraction of the PNS for higher values of m* owing to a decreased thermal pressure. These more compact PNSs also exhibit more neutrino heating, which drives earlier explosions and correlates with the GW amplitude via accretion plumes striking the PNS, exciting the oscillations. We investigate the spatial origin of the GWs and show the agreement between a frequency-radial distribution of the GW emission and a perturbation analysis. We do not rule out overshoot from below via PNS convection as another moderately strong excitation mechanism in our simulations. We also study the combined effect of effective mass and rotation. In all our simulations we find evidence for a power gap near ~1250 Hz; we investigate its origin and report its EOS dependence.

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Research Organization:: Michigan State Univ., East Lansing, MI (United States)

Sponsoring Organization:: USDOE Office of Science (SC), Nuclear Physics (NP); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR). Scientific Discovery through Advanced Computing (SciDAC); Swedish Research Council (SRC)

Grant/Contract Number:: SC0015904; SC0017955; 2016-07213

OSTI ID:: 1981233

Journal Information:: The Astrophysical Journal, Vol. 923, Issue 2; ISSN 0004-637X

Publisher:: IOP PublishingCopyright Statement

Country of Publication:: United States

Language:: English

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