Numerical-relativity simulation for tidal disruption of white dwarfs by a supermassive black hole
arXiv:2212.10891 · doi:10.1103/PhysRevD.107.043033
Abstract
We study tidal disruption of white dwarfs in elliptic orbits with the eccenticity of -- by a non-spinning supermassive black hole of mass in fully general relativistic simulations targeting the extreme mass-ratio inspiral leading eventually to tidal disruption. Numerical-relativity simulations are performed by employing a suitable formulation in which the weak self-gravity of white dwarfs is accurately solved. We reconfirm that tidal disruption occurs for white dwarfs of the typical mass of and radius \,km near the marginally bound orbit around a non-spinning black hole with $M_{\rm BH}\alt 4\times 10^5M_\odot$.
arXiv commentAccepted for publication in PRD
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