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While computing the Fermi degeneracy pressure of electrons in a white dwarfstar within the framework of hydrostatic equilibrium, we depart from the extantpractice of treating the electrons as a free fermion gas, by including theeffect of the star's self-gravity as an effective gravitational potential. Bythe star's self gravity, we mean the gravitational field due to the staritself, resulting from the mass of its constituent atoms, the mass of the atombeing effectively the mass of the proton. Modifying the free particleHamiltonian with this effective potential, we employ first order quantummechanical perturbation theory to compute the degeneracy pressure, in order tostudy the effect of inclusion of this self-gravity of the star on theChandrasekhar limiting mass. The final effect is found to be non-trivial, butperhaps a shade too small to alter any major observational result.

Self-gravity Correction to the Chandrasekhar Limiting Mass of White Dwarfs