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Type Ia supernovae (SNe Ia) originate from the thermonuclear explosion ofcarbon-oxygen white dwarfs (CO WDs), giving rise to luminous opticaltransients. A relatively common variety of subluminous SNe Ia events, referredto as SNe Iax, are believed to arise from the failed detonation of a CO WD. Inthis paper, we explore failed detonation SNe Ia in the context of thedouble-degenerate channel of merging white dwarfs. In particular, we havecarried out the first fully three-dimensional simulation of the merger of a ONeWD with a CO WD. While the hot, tidally-disrupted carbon-rich disk materialoriginating from the CO WD secondary is readily susceptible to detonation insuch a merger, the ONe WD primary core is not. This merger yields a faileddetonation, resulting in the ejection of a small amount of mass, and leavingbehind a kicked, super-Chandrasekhar ONe WD remnant enriched by the fallback ofthe products of nuclear burning. The resulting outburst is a rapidly-fadingoptical transient with a small amount of radioactive $^{56}$Ni powering thelight curve. Consequently, the ONe-CO WD merger naturally produces a very faintand rapidly-fading transient, fainter even than the faintest Type Iax eventsobserved to date, such as SN $2008$ha and SN 2010ae. More massive ONe primariesthan considered here may produce brighter and longer-duration transients.

Double-Degenerate Carbon-Oxygen and Oxygen-Neon White Dwarf Mergers: A New Mechanism for Faint and Rapid Type Ia Supernovae