  We run a suite of hydrodynamics simulations of tidal disruption events (TDEs)
of a white dwarf (WD) by a black hole (BH) with a wide range of WD/BH masses
and orbital parameters. We implement nuclear reactions to study nucleosynthesis
and its dynamical effect through release of nuclear energy. The released
nuclear energy effectively increases the fraction of unbound ejecta. This
effect is weaker for a heavy WD with 1.2 $\mathrm{M}_{\odot}$, because the
specific orbital energy distribution of the debris is predominantly determined
by the tidal force, rather than by the explosive reactions. The elemental yield
of a TDE depends critically on the initial composition of a WD, while the BH
mass and the orbital parameters also affect the total amount of synthesized
elements. Tanikawa et al. (2017) find that simulations of WD-BH TDEs with low
resolution suffer from spurious heating and inaccurate nuclear reaction
results. In order to examine the validity of our calculations, we compare the
amounts of the synthesized elements with the upper limits of them derived in a
way where we can avoid uncertainties due to low resolution. The results are
largely consistent, and thus support our findings. We find particular TDEs
where early self-intersection of a WD occurs during the first pericentre
passage, promoting formation of an accretion disc. We expect that relativistic
jets and/or winds would form in these cases because accretion rates would be
super-Eddington. The WD-BH TDEs result in a variety of events depending on the
WD/BH mass and pericentre radius of the orbit.
