Numerical-relativity simulation for tidal disruption of white dwarfs by a supermassive black hole

We study tidal disruption of white dwarfs in elliptic orbits with the eccenticity $\sim 1/3$--$2/3$ by a non-spinning supermassive black hole mass $M_{\rm BH}=10^5M_\odot$ fully general relativistic simulations targeting extreme mass-ratio inspiral leading eventually to disruption. Numerical-relativity are performed employing suitable formulation which weak self-gravity is accurately solved. reconfirm that occurs for typical 0.6M_\odot$ and radius $\approx 1.2 \times 10^4$\,km near marginally bound orbit around BH}\alt 4\times 10^5M_\odot$.