2005MNRAS.361..803F

We report the discovery of the nearby (d= 24 pc) HD 75767 as an eight billion year old quadruple system consisting of a distant M dwarf pair, HD 75767 C-D, in orbit around the known short-period P= 10.25 d single-lined binary HD 75767 A-B, the primary of which is a solar-like G star. On the reasonable assumption of synchronous orbital rotation as well as rotational and orbital coplanarity for the inner pair, we get M_B= 0.96M_☉ for the unseen HD 75767 B, that is, the case of a massive white dwarf. Upon future evolution, mass transfer towards HD 75767 B will render the M_A=0.96M_☉ G-type primary, now a turnoff star, to become a helium white dwarf of M_A∼0.33M_☉. Depending on the mass accretion rate, accretion efficiency and composition of the massive white dwarf, this in turn may result in a collapse of HD 75767 B with the formation of a millisecond pulsar, i.e. the creation of a low-mass binary pulsar (LMBP), or, instead, a Type Ia supernova explosion and the complete disruption of HD 75767 B. Irrespective of which scenario applies, we point to the importance of the distant M dwarfs as the likely agents for the formation of the inner, short-period HD 75767 A-B pair, and hence a path that particularly avoids preceding phases of common envelope evolution.