Numerical treatments in the different codes which are inherent to them.
|Single star prescriptions||HPT00||VB98||HPT00||HPT00|
|Stability of RLOF||q crit||Rconv, qcrit||ζ||ζ, q|
|Mass transfer rate||Rd/R||Rd/R||ζ →||ζ →|
|Wind (AGB)||R75, VW93, HPT00||HG97||R75, VW93, HPT00||R75, VW93, HPT00|
|AML (wind)||Donor (HTP02)||No||Donor||Donor|
|Helium star evolution||Yes||Not explicit||Yes||Yes|
|Population synthesis||Grid-based||Grid-based||Monte Carlo||Monte Carlo|
Notes.Further explanation can be found in Appendix B. (1) Mass ratio threshold for delayed dynamical instability (Hjellming & Webbink 1987), dependent on evolutionary state of the donor. (2) RRL is the Roche radius of the donor star. (3) τ∗ = Characteristic timescale of mass transfer. Can be nuclear, Kelvin-Helmholtz, timescale of magnetic braking or of gravitational wave radiation.
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