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We present an analysis of the close double degenerate NLTT 12758, which iscomprised of a magnetic white dwarf with a field of about 3.1 MG and anapparently non-magnetic white dwarf. We measured an orbital period of 1.154days and found that the magnetic white dwarf is spinning around its axis with aperiod of 23 minutes. An analysis of the atmospheric parameters has revealedthat the cooling ages of the two white dwarfs are comparable, suggesting thatthey formed within a short period of time from each other. Our modellingindicates that the non-magnetic white dwarf is more massive (M=0.83 M_sun) thanits magnetic companion (M=0.69 M_sun) and that the total mass of the system ishigher than the Chandrasekhar mass. Although the stars will not come intocontact over a Hubble time, when they do come into contact, dynamicallyunstable mass transfer will take place leading to either an accretion inducedcollapse into a rapidly spinning neutron star or a Type Ia supernova.

A fast spinning magnetic white dwarf in the double-degenerate, super-Chandrasekhar system NLTT 12758