  We present results from general relativistic calculations of the tidal
disruption of white dwarf stars from near encounters with intermediate mass
black holes. We follow the evolution of 0.2 and $0.6 M_\odot$ stars on
parabolic trajectories that approach $10^3$ - $10^4 M_\odot$ black holes as
close as a few Schwarzschild radii at periapsis, paying particular attention to
the effect tidal disruption has on thermonuclear reactions and the synthesis of
intermediate to heavy ion elements. These encounters create diverse
thermonuclear environments characteristic of Type I supernovae and capable of
producing both intermediate and heavy mass elements in arbitrary ratios,
depending on the strength (or proximity) of the interaction. Nuclear ignition
is triggered in all of our calculations, even at weak tidal strengths $\beta
\sim 2.6$ and large periapsis radius $R_P \sim 28$ Schwarzschild radii. A
strong inverse correlation exists between the mass ratio of calcium to iron
group elements and tidal strength, with $\beta \lesssim 5$ producing
predominately calcium-rich debris. At these moderate to weak interactions,
nucleosynthesis is not especially efficient, limiting the total mass and
outflows of calcium group elements to $< 15$\% of available nuclear fuel. Iron
group elements however continue to be produced in greater quantity and ratio
with increasing tidal strength, peaking at $\sim 60$\% mass conversion
efficiency in our closest encounter cases. These events generate short bursts
of gravitational waves with characteristic frequencies 0.1-0.7 Hz and strain
amplitudes $0.5\times10^{-22}$ - $3.5\times10^{-22}$ at 10 Mpc source distance.
