Equilibrium Configurations of Rotating White Dwarfs at Finite Temperatures

TL;DR

This paper investigates the equilibrium configurations of rotating white dwarfs at finite temperatures using classical physics, highlighting the importance of temperature and rotation effects on their structure and observational properties.

Contribution

It introduces a comprehensive analysis of hot and rotating white dwarfs using the Chandrasekhar equation of state and the Hartle approach, emphasizing the combined impact of temperature and rotation.

Findings

Finite temperature effects are crucial in low-mass white dwarfs.

Rotation significantly influences white dwarf structure across all masses.

Accounting for both temperature and rotation improves the modeling of observed white dwarf radii.

Abstract

In this work, cold and hot, static and rotating white dwarf stars are investigated within the framework of classical physics, employing the Chandrasekhar equation of state. The main parameters of white dwarfs such as the central density, pressure, total mass and radius are calculated fulfilling the stability criteria for hot rotating stars. To construct rotating configurations the Hartle approach is involved. It is shown that the effects of finite temperatures become crucial in low-mass white dwarfs, whereas rotation is relevant in all mass range. The simultaneous accounting for temperature and rotation is critical in the calculation of the radii of white dwarfs. The results obtained in this work can be applied to explain a variety of observational data for white dwarfs from the Sloan Digital Sky Survey Data Releases.