A general-relativistic extension of the classical Newtonian stellar structure equations, derived from a refined definition of quasi-local energy and mass. Unlike the standard treatment, which assumes the Newtonian approximation suffices for medium-density stars like the sun, these equations retain non-perturbative gravitational effects and predict that interior quantities (density, sound speed) follow power laws differing from the standard solar model. Students learn the relativistic hydrostatic equations, how they reduce to the Newtonian ones in the weak-field limit, and a resulting mass formula applied to the sun and gas planets.
A conference proceeding (Astronomische Nachrichten, 2025) reviewing the author's proposed relativistic extension of the classical stellar structure equations. General relativity has been applied in a…