白矮星由净电荷产生的额外压力

IF 2.2 4区 物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS Publications of the Astronomical Society of Japan Pub Date : 2023-08-09 DOI:10.1093/pasj/psad047
Ting-Han Pei
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引用次数: 0

摘要

基于绝对零度下理想简并费米电子气体,预测白矮星的质量上限为1.44 ${M}_{\odot} $。然而,应该考虑更多的条件,如温度和电荷。本研究首先利用统计力学中的大配分函数,建立了电子、气体压力和粒子数随温度的表达式。在1.16 × 107 K时,有大约1.50 × 10−4个电子超过费米能量,在1.16 × 104 K时,有大约1.50 × 10−7个电子超过费米能量。因为这些费米电子中的一些具有极强的相对论性,它们中的一些可以逃离引力,一些在离开恒星后回到恒星。这两种机制导致了带正电荷的恒星,而净正电荷产生了一种排斥力和对重力的压力。当恒星在1020℃带电时,增加的压力与T = 0时费米电子气体的压力相当,净电荷会降低恒星的质量密度,但会增加质量上限。
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The additional pressure of white dwarf stars generated by net charges
The upper-mass limit of a white dwarf star is predicted to be 1.44 ${M}_{\odot} $ based on an ideally degenerate Fermi electron gas at a temperature of absolute zero. However, more conditions should be considered, such as temperature and charge. In this research, first, we use the grand partition function in statistical mechanics to build expressions for the electron gas pressure and the particle number depending on temperature. At 1.16 × 107 K, there is a total of about 1.50 × 10−4 electrons exceeding the Fermi energy, and about 1.50 × 10−7 at 1.16 × 104 K. Because some of these Fermi electrons are extremely relativistic, some of them can escape the gravity and some return to the star after leaving. These two mechanisms result in a positively charged star and the net positive charges produce a repulsive force and pressure against gravity. The increased pressure is comparable to that of the Fermi electron gas at T = 0 when the star is charged at 1020 C. The net charges will decrease the mass density of the star but increase the upper-mass limit.
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来源期刊
Publications of the Astronomical Society of Japan
Publications of the Astronomical Society of Japan 地学天文-天文与天体物理
CiteScore
4.10
自引率
13.00%
发文量
98
审稿时长
4-8 weeks
期刊介绍: Publications of the Astronomical Society of Japan (PASJ) publishes the results of original research in all aspects of astronomy, astrophysics, and fields closely related to them.
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