The Significant Improvement of The Upper Mass Limit of The White Dwarf Star

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.

Comments: 16 Pages.

Download: PDF

Submission history

[v1] 2018-07-07 12:47:52
[v2] 2018-07-08 07:12:28
[v3] 2018-07-22 22:39:06
[v4] 2018-07-27 22:06:48
[v5] 2018-12-22 07:13:51

Unique-IP document downloads: 74 times is a pre-print repository rather than a journal. Articles hosted may not yet have been verified by peer-review and should be treated as preliminary. In particular, anything that appears to include financial or legal advice or proposed medical treatments should be treated with due caution. will not be responsible for any consequences of actions that result from any form of use of any documents on this website.

Add your own feedback and questions here:
You are equally welcome to be positive or negative about any paper but please be polite. If you are being critical you must mention at least one specific error, otherwise your comment will be deleted as unhelpful.

comments powered by Disqus