Characterizing the Gravitational Wave Signal from Core-collapse Supernovae

By David Radice, V. Morozova, Adam Burrows, D. Vartanyan, Hiroki Nagakura. Astrophysical Journal, 2018

175 citations recorded by the source corpus.

We study the gravitational wave (GW) signal from eight new 3D core-collapse supernova simulations. We show that the signal is dominated by f- and g-mode oscillations of the protoneutron star (PNS) and its frequency evolution encodes the contraction rate of the latter, which, in turn, is known to depend on the star’s mass, on the equation of state, and on transport properties in warm nuclear matter. A lower-frequency component of the signal, associated with the standing accretion shock instability, is found in only one of our models. Finally, we show that the energy radiated in GWs is proportional to the amount of turbulent energy accreted by the PNS.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0ea8e2ea4cb31ae8fd114fb9a5f6c926a4eee127

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Citations in the corpus

The overarching framework of core-collapse supernova explosions as revealed by 3D fornax simulations (2019, methodology): “M model do we see the original SASI mode (Blondin et al. 2003; Radice et al. 2019).”
Science case for the Einstein telescope (2019, background): “A general consensus from all modern numerical simulations is that the expected GW signal is weak (GW released energy of the order of 10−9 M c 2) [130].”