Abstract
The mass-radius relations for white dwarfs are investigated by solving the Newtonian as well as Tolman-Oppenheimer-Volkoff (TOV) equations for hydrostatic equilibrium assuming the electron gas to be non-interacting. We find that the Newtonian limiting mass of is modified to in the general relativistic case for (and ) white dwarfs. Using the same general relativistic treatment, the critical mass for white dwarfs is obtained as . In addition, departure from the ideal degenerate equation of state (EoS) is accounted for by considering Salpeter’s EoS along with the TOV equation, yielding slightly lower values for the critical masses, namely for , for and for white dwarfs. We also compare the critical densities for gravitational instability with the neutronization threshold densities to find that and white dwarfs are stable against neutronization with the critical values of and , respectively. However, the critical masses for , , , , and white dwarfs are lower due to neutronization. Corresponding to their central densities for neutronization thresholds, we obtain their maximum stable masses due to neutronization by solving the TOV equation coupled with the Salpeter EoS.
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