= Wind-loaded Keplerian disk evolution
{title2=$\Sigma_t=\frac3r\partial_r[\sqrt r\,\partial_r(\sqrt r\bar\nu\Sigma)]+\frac1r\partial_r[2(q-1)r^2S]-S$}
Subtract local <specific angular momentum> times <mass conservation> from <conservation of angular momentum> including wind losses S,T. With outward radial mass flux $\mathcal F$ and outward <viscous torque in an accretion disk> $\mathcal G=-2\pi\bar\nu\Sigma r^3\Omega'$, this gives $\mathcal Fh'+\mathcal G'=2\pi r(Sh-T)$. For <Keplerian rotation> and $T=qSh$, substitution in mass conservation yields the displayed equation. A wind with q=1 removes local angular momentum but supplies no additional drift term; q>1 can drive accretion even with zero viscosity.
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