Abstract
We present results from fully relativistic three-dimensional core-collapse supernova (CCSN) simulations of a non-rotating 15M⊙ star using three different nuclear equations of state (EoSs). From our simulations, we show that the development of the standing accretion shock instability (SASI) differs significantly depending on the stiffness of nuclear EoS. By evaluating the gravitational-wave (GW) emission, we find a new quasi-periodic GW signature on top of the previously identified high frequency (∼500–1000 Hz) one, which is originated from the g-mode oscillation of the photo-neutron star (PNS) surface. The newly found signal appears in relatively low frequency range from ∼100 to 200 Hz. By analyzing the cycle frequency of the SASI sloshing and spiral modes as well as the mass accretion rate to the emission region, we show that the SASI frequency is correlated with the newly found GW emission frequency. This is because the SASI-induced temporary perturbed mass accretion strikes the PNS surface leading to the quasi-periodic GW emission.
Highlights
Clarifying a correspondence between core-collapse supernova (CCSN) dynamics and the GW signals is a major challenge after the first detection coined by LIGO for the black hole merger event [1]
We present results from fully relativistic three-dimensional core-collapse supernova (CCSN) simulations of a non-rotating 15M⊙ star using three different nuclear equations of state (EoSs)
We show that the development of the standing accretion shock instability (SASI) differs significantly depending on the stiffness of nuclear EoS
Summary
Clarifying a correspondence between CCSN dynamics and the GW signals is a major challenge after the first detection coined by LIGO for the black hole merger event [1]. Most of the theoretical predictions have focused on the GW signals from rotational core collapse and bounce (see, e.g., [2, 3]). While in the non-rotating core model, the evolution of convective activities in the PNS surface regions are considered to be the primal emission mechanism as a result of the g-mode oscillation, whose frequency appears at relatively high region (∼ 500 − 1000 Hz) depending on the PNS surface properties [4]. Our results reveal a new GW signature where the SASI activity is imprinted
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