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Numerical relativity simulations of black hole and relativistic jet formation

MPS-Authors
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Kuroda,  Takami
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Shibata,  Masaru
Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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2404.02792.pdf
(Preprint), 391KB

slae069.pdf
(Publisher version), 777KB

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Citation

Kuroda, T., & Shibata, M. (2024). Numerical relativity simulations of black hole and relativistic jet formation. Monthly Notices of the Royal Astronomical Society: Letters, 533(1), L107-L112. doi:10.1093/mnrasl/slae069.


Cite as: https://hdl.handle.net/21.11116/0000-000F-BAA9-1
Abstract
We investigate impacts of stellar rotation and magnetic fields on black hole
(BH) formation and its subsequent explosive activities, by conducting
axisymmetric radiation-magnetohydrodynamics simulations of gravitational
collapse of a 70 $M_\odot$ star with two-moment multi energy neutrino transport
in numerical relativity. Due to its dense stellar structure, all models cannot
avoid the eventual BH formation even though a strongly magnetized model
experiences the so-called magnetorotational explosion prior to the BH
formation. One intriguing phenomenon observed in the strongly magnetized model
is the formation of a relativistic jet in the post-BH formation. The
relativistic jet is the outcome of a combination of strong magnetic fields and
low-density materials above the BH. The jet further enhances the explosion
energy beyond $\sim10^{52}$ erg, which is well exceeding the gravitational
overburden ahead of the shock. Our self-consistent supernova models demonstrate
that rotating magnetized massive stars at the high-mass end of supernova
progenitors could be a potential candidate of hypernova and long gamma-ray
burst progenitors.