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White dwarfs (WDs) are believed to detonate via explosive Carbon-fusion in aType Ia Supernova when their temperature and/or density reach the point whereCarbon is ignited in a runaway reaction. Observations of the Type Ia supernova(SN) rate imply all WD binaries that merge through the emission ofgravitational radiation within a Hubble time should result in SNe, regardlessof total mass. Here we investigate the conditions under which a single WD in abinary system might extract energy from its orbit, depositing enough energyinto a resonant mode such that it detonates before merger. We show that,ignoring non-linear effects, in a WD binary in tidal lock at small binaryseparations, the sustained tidal forcing of a low-order quadrupolar g-mode or aharmonic of a low-order quadrupolar p-mode could in principle drive the averagetemperature of Carbon nuclei in the mode over the runaway fusion threshold. Ifgrowing mode energy is thermalized at a core/atmosphere boundary, rapid Heliumburning and inward-travelling p-waves may result in core detonation.Thermalization at a boundary in the core can also result in detonation. Ifenergy can be efficiently transferred from the orbit to modes as the WD binarypasses through resonances, the WD merger timescale will be shortened by Myr-Gyrcompared to expected timescales from GW-emission alone and GW detectors willobserve deviations from predicted chirp profiles in resolved WD binaries.Future work in this area should focus on whether tidal locking in WD binariesis naturally driven towards low-order mode frequencies.

On the resonant detonation of sub-Chandrasekhar mass white dwarfs during binary inspiral