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 of $\sim 1\mathrm{/}3$–$2\mathrm{/}3$ by a non-spinning supermassive black hole of mass $M_{\mathrm{B}\mathrm{H}}={10}^5{M}_{\odot }$ 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 $M_{\mathrm{B}\mathrm{H}}\text{alt}4\times {10}^5{M}_{\odot }$.