= Hill-cloud transit mass estimate
{c}
{title2=$M_p/M_\star=3(\pi D/(\eta P))^3$}
For an opaque or detectably extinguishing spherical debris cloud of radius $R_c=\eta R_H$ much larger than the stellar radius, a central <exoplanet transit> lasts approximately $2R_c/(na)$. Combining this with the <Hill radius> gives the displayed mass estimate. For cloud impact distance $s$, replace $R_c$ by $\sqrt{R_c^2-s^2}$: the central formula then gives a lower mass estimate unless the chord geometry is known.
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