Stellar-mass scaling of radial-velocity planet estimates
= Stellar-mass scaling of radial-velocity planet estimates
At fixed observed period and semi-amplitude, $M_p\sin i\propto M_\star^{2/3}$ and $a\propto M_\star^{1/3}$. At fixed <planet> <mass> and amplitude threshold, the largest circular orbit instead scales as $M_\star^{-1}$. A revised stellar <radius> affects transit-derived <planet> radii but not these leading dynamical relations.