The Theory of Hot White Dwarfs Based on a Two-Component Equation of State

A variant of the theory of hot white dwarfs of small and intermediate masses is proposed using a model with a partially degenerate ideal relativistic electron gas and an ideal classical nuclear gas.  By modeling the radial temperature distribution, a reduced three-parameter equation of state was obtained as a function of matter density.  Based on numerically obtained solutions of the equilibrium equation, the characteristics of white dwarfs were determined as functions of the model parameters.  The inverse problem was solved – the values of the model parameters were calculated for a group of observed white dwarfs with effective temperatures $T_{\rm eff} \leq 8.8\cdot 10^4\,K$.

hot white dwarf
рівняння держави
mechanical equilibrium equation
stellar structure
internal structural properties
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