Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation
Abstract
We numerically study the collapse of rotating, very-massive stellar cores with masses of ≈ 200, $300$, $500$, and 1100M⊙ into black holes using both axisymmetric and three-dimensional (3D) numerical relativity. Our results indicate that when the dimensionless spin of the resulting black hole exceeds 0.8, a massive disk consistently forms around it. These massive, compact disks, carrying more than about 10\% of the black hole's mass, are prone to non-axisymmetric deformations that trigger gravitational-wave bursts with frequencies around 10-50 Hz. Such waves could be detected by the Einstein Telescope and Cosmic Explorer, even from sources a few Gpc away. We also summarize the gravitational-wave signals from axisymmetric collapse, which tend to have lower amplitudes and higher frequencies than those caused by non-axisymmetric instabilities.
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BibTeX
@misc{lam2026gravitational,
title = {{Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation}},
author = {Alan Tsz-Lok Lam and Masaru Shibata and Sho Fujibayashi},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.00200},
eprint = {2609.00200},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.00200},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation
AU - Alan Tsz-Lok Lam
AU - Masaru Shibata
AU - Sho Fujibayashi
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2609.00200
UR - https://arxiv.org/abs/2609.00200
AB - We numerically study the collapse of rotating, very-massive stellar cores with masses of ≈ 200, $300$, $500$, and 1100M_⊙ into black holes using both axisymmetric and three-dimensional (3D) numerical relativity. Our results indicate that when the dimensionless spin of the resulting black hole exceeds 0.8, a massive disk consistently forms around it. These massive, compact disks, carrying more than about 10\% of the black hole's mass, are prone to non-axisymmetric deformations that trigger gravitational-wave bursts with frequencies around 10-50 Hz. Such waves could be detected by the Einstein Telescope and Cosmic Explorer, even from sources a few Gpc away. We also summarize the gravitational-wave signals from axisymmetric collapse, which tend to have lower amplitudes and higher frequencies than those caused by non-axisymmetric instabilities.
ER -