Authors: Ting-Hang Pei
The upper mass limit of the white dwarf star is predicted 1.44 Mʘ based on the ideally degenerate Fermi electron gas at the temperature of absolute zero. However, more conditions should be considered like temperature and charges. In this research, first we use the grand partition function in statistical mechanics to build the expressions of the electron gas pressure and the particle number depending on temperature. At 1.16x1^07 K, there is about 1.50x10^-4 of total electrons exceeding the Fermi energy, and about 1.50x10^-7 at 1.16x10^4 K. Because some of this Fermi electron gas are the extremely relativistic electrons, some of them can escape the gravity and some return the star after leaving. These two mechanisms result in a positively charged star and the net positive charges produce the repulsive force and the pressure to against gravity. The increases pressure is comparable to that of the Fermi electron gas at T=0 when the star is charged at 10^20 C.
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