= Minimum companion mass from radial velocity
{title2=$M_p\sin i$}
For a companion of negligible <mass> compared with its host, $M_p\sin i=K[P/(2\pi G)]^{1/3}M_\star^{2/3}\sqrt{1-e^2}$. The observable supplies a projected <mass>; the minimum at a specified eccentricity occurs for an edge-on orbit. A <exoplanet transit> can constrain inclination, while low-inclination stars or brown dwarfs can otherwise mimic a lower-<mass> companion. The exact relation retains $(M_\star+M_p)^{2/3}$ in the denominator.
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