http://arxiv.org/abs/2212.10891
We study tidal disruption of white dwarfs in elliptic orbits with the eccenticity of $\sim 1/3$–$2/3$ by a non-spinning supermassive black hole of mass $M_{\rm BH}=10^5M_\odot$ 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 $\sim 0.6M_\odot$ and radius $\approx 1.2 \times 10^4$\,km near the marginally bound orbit around a non-spinning black hole with $M_{\rm BH}\alt 4\times 10^5M_\odot$.
A. Lam, M. Shibata and K. Kiuchi
Thu, 22 Dec 22
47/59
Comments: N/A