Low- and intermediate-mass close binary evolution and the initial-final mass relation - II. Non-conservative case with convective overshooting

Employing Eggleton's stellar evolution code, we carry out 150 runs of non-conservative population I binary evolution calculations with the initial primary mass between 1 and 8 M⊙, the initial mass ratio q=M1/M2 between 1.1 and 4 and the onset of Roche lobe overflow (RLOF) at early, middle or late Hertzsprung gap. Convective overshooting is included in our models and we assume that 50 per cent of the mass lost from the primary during the RLOF is accreted on to the secondary. The other 50 per cent is lost from the system, carrying away the same specific angular momentum as the centre of mass of the primary. We find that the remnant mass depends on when the RLOF begins in the Hertzsprung gap and the dependence increases with the primary mass. The remnant mass, however, does not depend much on the initial mass ratio, as in conservative cases. For qi= 1.1, we fit a formula for the remnant mass as a function of the initial mass M1i of the primary and the radius of the primary at the onset of RLOF with an error of less than 2.61 per cent. We have also discussed the influences of the convective overshooting that makes the helium burning and carbon burning earlier and the final mass of the primary larger (for M1i greater than 1.6 M⊙). The convective overshooting has no effect for low-mass binaries, consistent with the results of previous studies.