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Massive binaries are vital sources of various transient processes, includinggravitational-wave mergers. However, large uncertainties in the evolution ofmassive stars, both physical and numerical, present a major challenge to theunderstanding of their binary evolution. In this paper, we upgrade ourinterpolation-based stellar evolution code METISSE to include the effects ofmass changes, such as binary mass transfer or wind-driven mass loss, notalready included within the input stellar tracks. METISSE's implementation ofmass loss (applied to tracks without mass loss) shows excellent agreement withthe SSE fitting formulae and with detailed MESA tracks, except in cases wherethe mass transfer is too rapid for the star to maintain equilibrium. We usethis updated version of METISSE within the binary population synthesis code BSEto demonstrate the impact of varying stellar evolution parameters, particularlycore overshooting, on the evolution of a massive (25M$_\odot$ and 15M$_\odot$)binary system with an orbital period of 1800 days. Depending on the inputtracks, we find that the binary system can form a binary black hole or a blackhole-neutron star system, with primary(secondary) remnant masses rangingbetween 4.47(1.36)M$_\odot$ and 12.30(10.89)M$_\odot$, and orbital periodsranging from 6 days to the binary becoming unbound. Extending this analysis toa population of isolated binaries uniformly distributed in mass and orbitalperiod, we show that the input stellar models play an important role indetermining which regions of the binary parameter space can produce compactbinary mergers, paving the way for predictions for current and futuregravitational-wave observatories.

Modelling stellar evolution in mass-transferring binaries and gravitational-wave progenitors with METISSE