2002MNRAS.331.1027D

The evolution of helium stars with masses of 1.5-6.7M_☉ in binary systems with a 1.4-M_☉ neutron star companion is presented. Such systems are assumed to be the remnants of Be/X-ray binaries with B-star masses in the range 8-20M_☉ which underwent a case B or case C mass transfer and survived the common-envelope and spiral-in process. The orbital period is chosen such that the helium star fills its Roche lobe before the ignition of carbon in the centre. We distinguish case BA (in which mass transfer is initiated during helium core burning) from case BB (onset of Roche-lobe overflow occurs after helium core burning is terminated, but before the ignition of carbon). We found that the remnants of case BA mass transfer from 1.5-2.9M_☉ helium stars are heavy CO white dwarfs. This implies that a star initially as massive as 12M_☉ is able to become a white dwarf. CO white dwarfs are also produced from case BB mass transfer from 1.5-1.8M_☉ helium stars, while ONe white dwarfs are formed from 2.1-2.5M_☉ helium stars. Case BB mass transfer from more massive helium stars with a neutron star companion will produce a double neutron star binary. We are able to distinguish the progenitors of type Ib supernovae (as the high-mass helium stars or systems in wide orbits) from those of type Ic supernovae (as the lower-mass helium stars or systems in close orbits). Finally, we derive a `zone of avoidance' in the helium star mass versus initial orbital period diagram for producing neutron stars from helium stars.