Gravitational waves from core collapse supernovae

By K. Yakunin, P. Marronetti, A. Mezzacappa, S. Bruenn, Ching-Tsai Lee, M. A. Chertkow, W. Hix, J. Blondin, E. Lentz, O. E. Bronson Messer and 1 more. Classical and quantum gravity, 2010

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We present the gravitational wave signatures for a suite of axisymmetric core collapse supernova models with progenitor masses between 12 and 25 M⊙. These models are distinguished by the fact that they explode and contain essential physics (in particular, multi-frequency neutrino transport and general relativity) needed for a more realistic description. Thus, we are able to compute complete waveforms (i.e. through explosion) based on non-parameterized, first-principles models. This is essential if the waveform amplitudes and time scales are to be computed more precisely. Fourier decomposition shows that the gravitational wave signals we predict should be observable by AdvLIGO across the range of progenitors considered here. The fundamental limitation of these models is in their imposition of axisymmetry. Further progress will require counterpart three-dimensional models.

Subfields: Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/ce79290f5128e307f41c17439d77c61801e1b85f

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Citations in the corpus

A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE OF CORE-COLLAPSE SUPERNOVAE. III. GRAVITATIONAL WAVE SIGNALS FROM SUPERNOVA EXPLOSION MODELS (2012, methodology): “Contrary to what more energetic explosion models (Murphy et al. 2009; Yakunin et al. 2010) might suggest, strong GW emission in the high-frequency band late in the explosion phase appears to be possible for underenergetic supernovae.”
Expected properties of the first gravitational wave signal detected with pulsar timing arrays (2015, background): “…(Wald 1983; Maggiore 2008); from compact binaries (emitting GWs while inspiraling towards one another until coalescence, Peters & Mathews 1963), to asymmetric spinning compact stars (Van Den Broeck 2005), and catastrophic supernovae explosions (Yakunin et al. 2010), just to mention a few.”
Non-Radial Instabilities and Progenitor Asphericities in Core-Collapse Supernovae (2014, background): “…years, an impressive set of successful two-dimensional (2D) multi-group neutrino hydrodynamics simulations (Buras et al. 2006a; Marek & Janka 2009; Yakunin et al. 2010; Suwa et al. 2010; Müller, Janka & Marek 2012; Müller, Janka & Heger 2012; Janka et al. 2012; Bruenn et al. 2013; Suwa et al.…”
Multiple physical elements to determine the gravitational-wave signatures of core-collapse supernovae (2011, methodology): “urface areas facing an observer adds up incoherently, so that the measurable modulation amplitudes of the GW signals (as well as neutrinos) are signiﬁcantly smaller than predicted by 2D si mulations ([129, 89]). The eﬀects of stellar rotation on the stochastic nature of the GWs have been recently st”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, methodology): “…our treatment of the microphysics and the neutrino transport is on par with previous works on the GW signal from 2D simulations (Marek et al. 2009; Yakunin et al. 2010; M¨uller et al. 2013; Yakunin et al. 2015), we were in the position to conduct a meaningful comparison of GW emission in 2D and…”
Prospects for Observing and Localizing Gravitational-Wave Transients with Advanced LIGO and Advanced Virgo (2013, background): “For example, GWs emitted by various processes in core-collapse supernovae are anticipated to have relatively large bandwidths, between 150 – 500 Hz [48, 82, 113, 83], largely independent of detector configuration.”
THREE-DIMENSIONAL HYDRODYNAMIC CORE-COLLAPSE SUPERNOVA SIMULATIONS FOR AN 11.2 M☉ STAR WITH SPECTRAL NEUTRINO TRANSPORT (2011, methodology): “By implementing a multi-group flux-limited diffusion algorithm to the CHIMERA code (e.g., Bruenn et al. 2010), Yakunin et al. (2010) obtained explosions for a non-rotating progenitorsof Woosley et al. (2002) in the mass range of 12M⊙ and 25M⊙.”
The Gravitational Wave Signal from Core-collapse Supernovae (2018, methodology): “…early ∼100 Hz signal arising in the first tens of milliseconds after core bounce is commonly associated with the shock oscillations driven by prompt convection (Marek et al. 2009; Murphy et al. 2009; Müller et al. 2013; Yakunin et al. 2010, 2015), which makes its parameterization very difficult.”