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首页> 外文期刊>Journal of Experimental and Theoretical Physics >Thermodynamic functions of degenerate magnetized electron gas
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Thermodynamic functions of degenerate magnetized electron gas

机译：简并磁化电子气的热力学函数

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摘要

The Fermi energy, pressure, internal energy, entropy, and heat capacity of completely degenerate relativistic electron gas are calculated by numerical methods. It is shown that the maximum admissible magnetic field on the order of 10 ~9 G in white dwarfs increases the pressure by a factor of 1.06 in the central region, where the electron concentration is ～10 ~(33) cm ~(-3), while the equilibrium radius increases by approximately a factor of 1.03, which obviously cannot be observed experimentally. A magnetic field of ～10 ~8 G or lower has no effect on the pressure and other thermodynamic functions. It is also shown that the contribution of degenerate electron gas to the total pressure in neutron stars is negligible compared to that of neutron gas even in magnetic fields with a maximum induction ～10 ~(17) G possible in neutron stars. The neutron beta-decay forbiddeness conditions in a superstrong magnetic field are formulated. It is assumed that small neutron stars have such magnetic fields and that pulsars with small periods are the most probable objects that can have superstrong magnetic fields.
机译：完全退化的相对论电子气的费米能，压力，内能，熵和热容通过数值方法计算。结果表明，在白矮星中最大允许磁场为10〜9 G量级，在中心区域，电子浓度为〜10〜（33）cm〜（-3），压力增加了1.06倍。 ，而平衡半径则增加了大约1.03倍，这显然无法通过实验观察到。 〜10〜8 G或更低的磁场对压力和其他热力学功能没有影响。研究还表明，即使在中子星最大感应强度约为10〜（17）G的磁场中，与中子气体相比，简并电子气对中子星总压力的贡献微不足道。制定了超强磁场中的中子β衰变禁忌条件。假定小中子星具有这样的磁场，而周期短的脉冲星是最可能具有超强磁场的物体。

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