= Isotropic stellar mass loss
{title2=$\ddot{\mathbf r}=-\mu(t)\mathbf r/r^3$}
<Isotropic stellar mass loss> changes the central gravitational parameter $\mu(t)$ while preserving the central direction of the force, provided the escaping material causes no recoil or drag on the orbiting body. The relative equation is $\ddot{\mathbf r}=-\mu(t)\mathbf r/r^3$. <Specific angular momentum> remains exactly constant; <specific orbital energy> obeys $\dot C=-\dot\mu/r$. Orbital expansion is adiabatic only when the <mass>-loss law varies slowly on the <orbital period>.
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