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The evolution of the remnant of the merger of two white dwarfs is still anopen problem. Furthermore, few studies have addressed the case in which theremnant is a magnetic white dwarf with a mass larger than the Chandrasekharlimiting mass. Angular momentum losses might bring the remnant of the merger tothe physical conditions suitable for developing a thermonuclear explosion.Alternatively, the remnant may be prone to gravitational or rotationalinstabilities, depending on the initial conditions reached after thecoalescence. Dipole magnetic braking is one of the mechanisms that can drivesuch losses of angular momentum. However, the timescale on which these lossesoccur depend on several parameters, like the strength of the magnetic field. Inaddition, the coalescence leaves a surrounding Keplerian disk that can beaccreted by the newly formed white dwarf. Here we compute the post-mergerevolution of a super-Chandrasekhar magnetized white dwarf taking into accountall the relevant physical processes. These include magnetic torques acting onthe star, accretion from the Keplerian disk, the threading of the magneticfield lines through the disk, as well as the thermal evolution of the whitedwarf core. We find that the central remnant can reach the conditions suitableto develop a thermonuclear explosion before other instabilities (such as theinverse beta-decay instability or the secular axisymmetric instability) arereached, which would instead lead to gravitational collapse of the magnetizedremnant.

The Spin Evolution of Fast-Rotating, Magnetized Super-Chandrasekhar White Dwarfs in the Aftermath of White Dwarf Mergers