Mass-shedding limit (${\Omega }_{\mathrm{shed}}\sim (GM/R_{\ast }^3{)}^{1/2}$)

The mass-shedding limit is the spin at which equatorial surface matter can no longer remain attached in equilibrium. Newtonian gravity gives a Keplerian frequency scale at the surface. Rotation-induced deformation, general relativity and the equation of state change the numerical bound. A magnetic-equilibrium formula is not valid indefinitely as the exterior magnetosphere shrinks inside the star.