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In this paper, we model the observable signatures of tidal disruptions ofwhite dwarf (WD) stars by massive black holes (MBHs) of moderate mass, $\approx10^3 - 10^5 M_\odot$. When the WD passes deep enough within the MBH's tidalfield, these signatures include thermonuclear transients from burning duringmaximum compression. We combine a hydrodynamic simulation that includes nuclearburning of the disruption of a $0.6 M_\odot$ C/O WD with a Monte Carloradiative transfer calculation to synthesize the properties of a representativetransient. The transient's emission emerges in the optical, with lightcurvesand spectra reminiscent of type I SNe. The properties are stronglyviewing-angle dependent, and key spectral signatures are $\approx 10,000$ kms$^{-1}$ Doppler shifts due to the orbital motion of the unbound ejecta.Disruptions of He WDs likely produce large quantities of intermediate-masselements, offering a possible production mechanism for Ca-rich transients.Accompanying multiwavelength transients are fueled by accretion and arise fromthe nascent accretion disk and relativistic jet. If MBHs of moderate mass existwith number densities similar to those of supermassive MBHs, both high energywide-field monitors and upcoming optical surveys should detect tens to hundredsof WD tidal disruptions per year. The current best strategy for their detectionmay therefore be deep optical follow up of high-energy transients ofunusually-long duration. The detection rate or the non-detection of thesetransients by current and upcoming surveys can thus be used to place meaningfulconstraints on the extrapolation of the MBH mass function to moderate masses.

Optical Thermonuclear Transients From Tidal Compression of White Dwarfs as Tracers of the Low End of the Massive Black Hole Mass Function