The radius variations of accreting main sequence stars and mass transfer instability
arxiv(2024)
摘要
Many previous works studied the dynamical timescale mass transfer stability
criteria based on the donor response with neglecting the stellar structure of
the accretor. In this letter, we investigate the radial response of accretors
with mass accumulation and its effect on the binary mass transfer stability. We
perform a series of detailed stellar evolution simulations with different types
of accretors and obtain the radial variations of stars accreting at different
rates. Since the time within which the donor loses half of the original mass
has a correlation with the donor mass, we approximately obtain the mean mass
transfer rate as a function of mass ratio. Assuming that the common envelope
(CE) phase occurs if the accretor radius exceeds the outer Roche lobe radius,
we obtain the critical mass ratio of dynamically unstable mass transfer. We
find the critical mass ratios for donors filling their Roche lobes at the Main
Sequence (MS) and Hertzsprung Gap (HG) stages are smaller than that derived
from the radial response of the donor in the traditional way. Our results may
suggest that the binary is easier to enter into the CE phase for a donor star
at the MS or HG stage than previously believed.
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