2001A&A...376L...9E

We investigate the evolution of a binary system which initially has an orbital period of 2^h17^m and contains a 0.5M_☉ helium star with a white dwarf companion of 0.97M_☉, similar to the suggested SNIa candidate progenitor KPD 1930+2752. We show that the helium star completes core helium burning and becomes a white dwarf before the components merge. The most probable outcome of the merger of the components is the formation of a massive white dwarf, despite the fact that initially the total mass of the system is above the Chandrasekhar mass.