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Fig. 8

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Mass transfer rates for a zero-temperature helium white dwarf donor with an initially 1.4 M, 12   km radius neutron star accretor (lower solid curve) and a 10 M black hole accretor (upper solid curve), starting at the dynamical instability limit (i.e. ignoring possible merging), for full feedback. The dashed curves branching away from these represent the evolution assuming no feedback below q = 0.01 (Sect. 4.1). The numbers correspond to the two circles on their left-hand side and represent the logarithm of the system age (yr), which is the time since the onset of mass transfer. Indicated are the isotropic re-emission regime (dashed, Eq. (11)), the Eddington limit (dotted) and the accretion disk instability limit by in’t Zand et al. (2007) (dash-dotted, Sect. 3.5) Note that the dashed neutron star curve at its local maximum “touching” the upper dash-dotted curve is a coincidence.

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