= Donor-wind angular-momentum loss
{title2=$\dot J=(1-f)\dot M_d a_d^2\Omega$}
An isotropic escaping <stellar wind> has the <donor star>'s mean specific orbital <angular momentum>. With $\dot M_d<0$, retained fraction $f$, negligible spin and no additional wind torque, $\dot J=(1-f)\dot M_da_d^2\Omega$. The retained matter redistributes <angular momentum> internally. Unlike <isotropic re-emission from a binary star>, the escaping material originates at the donor rather than the accretor. With no retention this reduces to <Jeans-mode mass loss>.
Back to article page
