Criterion for dynamical instability of mass transfer in binary evolution by Han, Z, Podsiadlowski, P, Tout, C

“…We found that the critical mass ratio, above which mass transfer is dynamically unstable, is from 1.1 to 1.3 in these red-giant binary systems.…”

The progenitors of type Ia supernovae by Tout, C, Regos, E, Wickramasinghe, D, Hurley, JR, Pols, O

“…Based on detailed binary star population synthesis calculations we propose that many SNe la could be such ELDs of CO white dwarfs that have accreted a critical mass of helium. Both the actual mass of the ELD and its composition, a function of its progenitor's mass, can affect its peak luminosity and light curve shape. …”

The structure and evolution of Thorne-Zytkow objects by Podsiadlowski, P

“…The TZO phase ends when either the star has exhausted its rp-process seed elements or the envelope mass decreases below a critical mass (similar to 14 M.). Then nuclear burning becomes inefficient and a neutrino runaway ensues, leading to the dynamical accretion of matter near the core onto the neutron star and its spin up to spin frequencies of up to similar to 100 Hz. …”