Using the hydrostatic law for a uniform density star gives the stellar pressure as a function of radius r as

where is the density,G is the gravitational constant,and R is the stellar radius.Applying the ideal gas law at the star's center then gives

where m is the molecular mass and k is Boltzmann's constant. Therefore, assuming only hydrostatic equilibrium (i.e., ignoring thermonuclear fusion), the temperature at the center of the star is

where M is the mass of the star.