= Independent-volume supernova quenching
{title2=$q(e^{\nu t}-1)=B(r)$}
Before local expulsion, a linear star-formation law $\psi=\nu\rho_g$ without return gives $\rho_g=\rho_0e^{-\nu t}$. If $q=\gamma E_{\rm SN}$ is the <energy> supplied per unit stellar <mass>, accumulated <energy> is $q\rho_0(1-e^{-\nu t})$. A fixed <binding energy> per unit remaining gas <mass> $B(r)$ gives the threshold $q(e^{\nu t}-1)=B(r)$. This assumes a specified retained gravitational profile and neglects exchange between <volumes>.
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