  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
$M_{\rm BH}\alt 4\times 10^5M_\odot$.
