期刊
ASTROPHYSICAL JOURNAL
卷 861, 期 1, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/aac5f1
关键词
equation of state; gravitational waves; hydrodynamics; supernovae: general
资金
- U.S. NSF [AST-1714267]
- Max-Planck/Princeton Center (MPPC) for Plasma Physics [PHY-1144374, PHY-1523261]
- DOE SciDAC4 [DE-SC0018297, 00009650]
- Princeton Institute for Computational Science and Engineering (PICSciE)
- Princeton University Office of Information Technology
- Office of Science of the U.S. Department of Energy (DOE) [DE-AC03-76SF00098]
- Frank and Peggy Taplin Membership at the Institute for Advanced Study
We study gravitational waves (GWs) from a set of 2D multigroup neutrino radiation hydrodynamic simulations of core-collapse supernovae (CCSNe). Our goal is to systematize the current knowledge about the post-bounce CCSN GW signal and recognize the templatable features that could be used by the ground-based laser interferometers. We demonstrate that, starting from similar to 400 ms after core bounce, the dominant GW signal represents the fundamental quadrupole (l = 2) oscillation mode (f-mode) of the proto-neutron star (PNS), which can be accurately reproduced by a linear perturbation analysis of the angle-averaged PNS profile. Before that, in the time interval between similar to 200 and similar to 400 ms after bounce, the dominant mode has two radial nodes and represents a g-mode. We associate the high-frequency noise in the GW spectrograms above the main signal with p-modes, while below the dominant frequency there is a region with very little power. The collection of models presented here summarizes the dependence of the CCSN GW signal on the progenitor mass, equation of state, many-body corrections to the neutrino opacity, and rotation. Weak dependence of the dominant GW frequency on the progenitor mass motivates us to provide a simple fit for it as a function of time, which can be used as a prior when looking for CCSN candidates in the LIGO data.
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