= Stellar radius from transit duration and a linear mass-radius relation
{title2=$R_\star/R_\odot=[A_\odot/(a/R_\star)]^{3/2}$}
Assume <Kepler's third law>, a negligible planet <mass>, and $M_\star/M_\odot=R_\star/R_\odot$. Define $A_\odot=[(GM)_\odot P^2/(4\pi^2)]^{1/3}/R_\odot$. The <total duration of a circular planetary transit> determines $a/R_\star$, giving the displayed <stellar radius>. Unknown <orbital eccentricity>, <transit dilution> or a different stellar mass-radius calibration introduces additional uncertainty.
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