arXiv (OAI Expanded)
open access
Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation
We numerically study the collapse of rotating, very-massive stellar cores with masses of $\approx 200$, $300$, $500$, and $1100M_\odot$ into black holes using both axisymmetric and three-dimensional (3D) numerical relativity. Our results indicate that when the dimensionless spin of the resulting bla
Conceptio Open Archive
Analyze & explore related research in Conceptio
Connect this record directly into your research workflow or AI agent. Explore citations across open repositories, query full text, and export structured proof bundles.
This document is indexed with metadata only: full text is not available in the archive for this record. Open the official source ↗
Related documents
- Gravitational waves from core collapse of rotating very-massive stars: 3D numerical relativity computation#819663
- Stochastic gravitational-wave background from subsolar neutron stars in collapsar disks#1130847
- Gravitational wave signatures of subsolar neutron star formation in collapsar disks#1051718
- Spin wandering of an accreting neutron star near torque balance: implications for gravitational wave searches#1116495
- Quasinormal modes of Reissner-Nordström black hole from bound state spectrum#1084881
Record · ID 809667
Retrieved via Conceptio: every document is proof-bundled with source, license, and retrieval metadata.
Retrieved via Conceptio: every document is proof-bundled with source, license, and retrieval metadata.
Bring this data into your agent: Connect via MCP or API · 20 free credits to start · no card required
Read the Docs → · View CLI source on GitHub · Conceptio Open Knowledge Archive
Read the Docs → · View CLI source on GitHub · Conceptio Open Knowledge Archive