恒星：演化、稳定性与统计力学
Stars: Evolution, Stability and Statistical Mechanics
AI总结：
本文利用热力学与统计力学综述恒星的结构、演化与稳定性，重点推导白矮星和中子星的最大质量极限，并阐明简并压力平衡引力收缩的机制，最后引入光度与辐射转移方程。
摘要：
本文综述了恒星的物理特性、类型、结构、演化与稳定性。利用简单的热力学和统计力学原理，揭示了白矮星和中子星的内部工作机制。本文主要聚焦于白矮星，但在某些部分，也提及了中子星，因为相关关系可以容易地推广到后者。可以证明，每种类型的恒星都存在一个最大质量极限，该极限可以被严格推导出来。利用最大熵原理可以表明，在白矮星的情形下，引力收缩被电子产生的简并压力所平衡；而在中子星中，该平衡由构成其物质的中子和质子所产生的简并压力实现。最后，本文引入了描述恒星光度及辐射转移的动力学方程。
英文摘要：
This paper reviews the physics of stars, the type, structure, evolution and stability. Simple thermodynamics and statistical mechanics are used to show the inner working of white dwarf and neutron stars. The major concentration of the paper will be on white dwarf stars although in some places references will also be made to neutron stars where the relations can be extended easily. It can be shown that a maximum mass limit is attached to each type of star which can be derived rigorously. Maximum entropy can be used to show that the gravitational contraction is balanced by the degeneracy pressure created by the electrons in the case of white dwarfs, and neutrons and protons which constitute the matter of the neutron star. Finally the kinetic equations which describe the luminosity of the star and the radiative transfer are introduced.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
