Numerical relativity simulations of black hole and relativistic jet formation
arxiv(2024)
摘要
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_⊙ 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 ∼10^52 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.
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