Gravitational Wave Emission from Core Collapse of Massive Stars

By Chris L. Fryer, D. Holz, S. Hughes. 2001

147 citations recorded by the source corpus.

We derive estimates for the characteristics of gravitational radiation from stellar collapse, using recent models of the core collapse of Chandrasekhar-massed white dwarfs (accretion-induced collapse), core-collapse supernovae and collapsars, and the collapse of very massive stars (≳300 M☉). We study gravitational wave emission mechanisms using several estimation techniques, including two-dimensional numerical computation of quadrupole wave emission, estimates of bar-mode strength, estimates of r-mode emission, and estimates of waves from black hole ringing. We also review the rate at which the relevant collapses are believed to occur, which has a major impact on their relevance as astrophysical sources. Although the latest supernova progenitor simulations produce cores rotating much slower than those used in the past, we find that bar-mode and r-mode instabilities from core-collapse supernovae remain among the leading candidate sources for second-generation detectors at the Laser Interferometer Gravitational-Wave Observatory (LIGO II). Accretion-induced collapse (AIC) of a white dwarf could produce gravitational wave signals similar to those from core collapse. In the models that we examine, such collapses are not unstable to bar modes; we note that models recently examined by Liu & Lindblom, which have slightly more angular momentum, are certainly unstable to bar formation. Because AIC events are probably 1000 times less common than core-collapse supernovae, the typical AIC event will be much farther away, and thus the observed waves will be much weaker. In the most optimistic circumstances, we find that it may be possible to detect gravitational waves from the collapse of 300 M☉ Population III stars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f46ddcbdc37dc969832360ac8e88d80a672d0c71

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Citations in the corpus

The THESEUS space mission concept: science case, design and expected performances (2017, background): “For long GRBs, joint THESEUS and GW/neutrino observations would further constrain progenitor models, clarifying the fraction of energy channeled via dynamical instabilities (Fryer et al., 2002) and the relative neutrino/EM energy budgets.”
A COMPARISON OF TWO- AND THREE-DIMENSIONAL NEUTRINO-HYDRODYNAMICS SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2013, background): “…that hydrodynamic motions associated with neutrino-driven convection (e.g., Herant et al. (1994); Burrows et al. (1995); Janka & Müller (1996); Fryer et al. (2002) and see collective references in Burrows et al. (2012); Murphy et al. (2013); Couch (2013)) and the SASI (e.g., Blondin et al.…”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, methodology): “, [52, 53, 54, 55, 56]) as well as the Standing-Accretio n-Shock-Instability (SASI, e.”
Modules for Experiments in Stellar Astrophysics ( ): Convective Boundaries, Element Diffusion, and Massive Star Explosions (2017, background): “…hole systems (Abbott et al. 2016a, 2016b, 2016c, 2017a, 2017b) and continues to monitor the sky with broadband detectors for gravitational waves from compact binary inspirals and asymmetrical exploding massive stars (Fryer et al. 2002; Gossan et al. 2016; Abbott et al. 2017a, 2016d, 2016e, 2016f).”
Equation-of-state dependent features in shock-oscillation modulated neutrino and gravitational-wave signals from supernovae (2008, background): “…convection inside the nascent neutron star can account for sizable gravitational-wave signals, which should be detectable with a high probability from a Galactic supernova when the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO II) is running (see also Fryer et al. 2002, 2004).”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, methodology): “To take into account the feedback between the mass accretion and the neutrino luminosity, the spectral IDSA scheme, which is beyond the grey transport scheme (e.g., Fryer et al. (2002); Fryer (2004)), sounds quite efficient in the first-generation 3D simulations.”
The basics of gravitational wave theory (2005, background): “ing during collapse, then instabilities may develop which lead to strong GW emission [70]. If such instabilities develop, core collapse GWs could be detected from events as far away as 10 Megaparsecs [71], a distance encompassing enough galaxies that several events per year would be likely. Most mod”
Toward Gravitational Wave Signals from Realistic Core-Collapse Supernova Models (2003, background): “…stellar models, and Newtonian gravity (Müller 1982; Finn & Evans 1990; Mönchmeyer et al. 1991; Yamada & Sato 1995; Zwerger & Müller 1997; Rampp et al. 1998; Dimmelmeier et al. 2002; Fryer et al. 2002, 2003; Imamura et al. 2003; Kotake, Yamada, & Sato 2003; Ott et al. 2004; Shibata 2003).”
Gamma-Ray Bursts in the Swift Era (2007, background): “…candidates for GRBs, i.e. mergers of binary compact objects (Thorne 1987; Phinney 1991; Kochanek & Piran 1993; Kobayashi & Mészáros 2003) and stellar core-collapses (Rampp et al. 1998; van Putten 2001; Fryer et al. 2002; Kobayashi & Mészáros 2003), have been suggested as potential GW sources.”