Laplace radius ($a_L=[2J_2(M_p/M_{\star })R_p^2{a}_p^3{]}^{1/5}$)

The Laplace radius is the satellite distance where the small-tilt nodal precession contributions from a planet's axisymmetric quadrupole and the stellar tide have equal magnitudes. In the circular hierarchical limit those rates are $3G{M}_p{J}_2{R}_p^2/(2n{a}^5)$ and $3G{M}_{\star }/(4n{a}_p^3)$. Equating them proves the displayed fifth-root expression. Inside this radius the planetary quadrupole coefficient controls the preferred plane; outside it the double-averaged circular tidal potential dominates. When equator and planetary orbit are inclined to one another, their balance determines the local Laplace plane.