Gravitational Waves from Core-Collapse Supernovae: Dependence on the Progenitor Star, Rotation Rate and Nuclear Equation of State
Abstract
We simulate 137 axisymmetric core-collapse supernova explosions to systematically investigate the impact of different progenitor properties, rotation rates, and equations of state on the supernova gravitational-wave emission. We use 15 different progenitor stars, with masses ranging from 9.71 M⊙ to 36.61 M⊙, three equations of state, and three rotation rates, with durations extending up to 5.5\,s after bounce. We find substantial differences in the gravitational-wave emission between equations of state, with the CMF equation of state producing lower gravitational-wave amplitudes and a longer low frequency mode due to the standing accretion shock instability that remains visible even at ∼5\,s post bounce. Rapid rotation also significantly alters the gravitational-wave signal, with more visible modes in the gravitational-wave emission, and lower energies due to later shock revival times. We include the gravitational-wave emission due to neutrino memory, and show it can significantly improve the detectability of core-collapse supernovae for observatories with improved low frequency sensitivity. We propose a recalibration of universal relations for the high frequency mode, using fits to our waveforms, that reduces the fit error at late times in the gravitational-wave signal. Finally, we investigate, for the first time, the impact of random seed perturbations on the gravitational-wave emission. We find that stochastic perturbations can produce dramatic variations in gravitational-wave amplitude, and can alter the signal-to-noise ratio of a detection by as much as 62\% for models close to the boundary between failed and successful shock revival.
Related
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BibTeX
@misc{powell2026gravitational,
title = {{Gravitational Waves from Core-Collapse Supernovae: Dependence on the Progenitor Star, Rotation Rate and Nuclear Equation of State}},
author = {Jade Powell and Bailey Sykes and Bernhard Müller},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.34405},
eprint = {2609.34405},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.34405},
}
RIS
TY - UNPB
TI - Gravitational Waves from Core-Collapse Supernovae: Dependence on the Progenitor Star, Rotation Rate and Nuclear Equation of State
AU - Jade Powell
AU - Bailey Sykes
AU - Bernhard Müller
PY - 2026
DA - 2026/09/28
PB - arXiv
DO - 10.48550/arxiv.2609.34405
UR - https://arxiv.org/abs/2609.34405
AB - We simulate 137 axisymmetric core-collapse supernova explosions to systematically investigate the impact of different progenitor properties, rotation rates, and equations of state on the supernova gravitational-wave emission. We use 15 different progenitor stars, with masses ranging from 9.71 M_⊙ to 36.61 M_⊙, three equations of state, and three rotation rates, with durations extending up to 5.5\,s after bounce. We find substantial differences in the gravitational-wave emission between equations of state, with the CMF equation of state producing lower gravitational-wave amplitudes and a longer low frequency mode due to the standing accretion shock instability that remains visible even at ∼5\,s post bounce. Rapid rotation also significantly alters the gravitational-wave signal, with more visible modes in the gravitational-wave emission, and lower energies due to later shock revival times. We include the gravitational-wave emission due to neutrino memory, and show it can significantly improve the detectability of core-collapse supernovae for observatories with improved low frequency sensitivity. We propose a recalibration of universal relations for the high frequency mode, using fits to our waveforms, that reduces the fit error at late times in the gravitational-wave signal. Finally, we investigate, for the first time, the impact of random seed perturbations on the gravitational-wave emission. We find that stochastic perturbations can produce dramatic variations in gravitational-wave amplitude, and can alter the signal-to-noise ratio of a detection by as much as 62\% for models close to the boundary between failed and successful shock revival.
ER -