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 eccentricity of-1/3-2/3 by a nonspinning supermassive black hole of mass MBH = 105M0 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-0.6M0 and radius c.-.,1.2 x 104 km near the marginally bound orbit around a nonspinning black hole with MBH less than or similar to 4 x 105M0.