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In this work, cold and hot, static and rotating white dwarf stars areinvestigated within the framework of classical physics, employing theChandrasekhar equation of state. The main parameters of white dwarfs such asthe central density, pressure, total mass and radius are calculated fulfillingthe stability criteria for hot rotating stars. To construct rotatingconfigurations the Hartle approach is involved. It is shown that the effects offinite temperatures become crucial in low-mass white dwarfs, whereas rotationis relevant in all mass range. The simultaneous accounting for temperature androtation is critical in the calculation of the radii of white dwarfs. Theresults obtained in this work can be applied to explain a variety ofobservational data for white dwarfs from the Sloan Digital Sky Survey DataReleases.

Equilibrium Configurations of Rotating White Dwarfs at Finite Temperatures