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 \times 10 ^ { -22 } - 3.5 \times 10 ^ { -22 } at 10 Mpc source distance .