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We consider tidal encounters between a white dwarf and an intermediate massblack hole. Both weak encounters and those at the threshold of disruption aremodeled. The numerical code combines mesh-based hydrodynamics, a spectralmethod solution of the self-gravity, and a general relativistic Fermi normalcoordinate system that follows the star and debris. Fermi normal coordinatesprovide an expansion of the black hole tidal field that includes quadrupole andhigher multipole moments and relativistic corrections. We compute the mass lossfrom the white dwarf that occurs in weak tidal encounters. Secondly, we computecarefully the energy deposition onto the star, examining the effects ofnonradial and radial mode excitation, surface layer heating, mass loss, andrelativistic orbital motion. We find evidence of a slight relativisticsuppression in tidal energy transfer. Tidal energy deposition is compared toorbital energy loss due to gravitational bremsstrahlung and the combined lossesare used to estimate tidal capture orbits. Heating and partial mass strippingwill lead to an expansion of the white dwarf, making it easier for the star tobe tidally disrupted on the next passage. Finally, we examine angular momentumdeposition. By including the octupole tide, we are able for the first time tocalculate deflection of the center of mass of the star and debris. With thisobserved deflection, and taking into account orbital relativistic effects, wecompute directly the change in orbital angular momentum and show its balancewith computed spin angular momentum deposition.

Relativistic effects in the tidal interaction between a white dwarf and a massive black hole in Fermi normal coordinates