Thermodynamics of neutrons in a magnetic field and its implications for neutron stars
Thermodynamics of neutrons in a magnetic field and its implications for neutron stars
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DOI：
10.1103/physrevc.99.065803
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发表时间：
2019-03
影响因子：
3.1
通讯作者：
E. J. Ferrer;A. Hackebill
中科院分区：
文献类型：
--
作者：
E. J. Ferrer;A. Hackebill
我们研究了在有限密度和温度下磁场对中子系统热力学的影响。我们的主要动机是加深对一类被称为磁星的中子星的物理理解，这种中子星显示出极强的磁场。考虑到两个事实：(I)磁场存在压力各向异性；(Ii)量子场论对压强的贡献是不可忽略的。我们证明，在满足引力和物质压强之间的磁流体静力平衡的情况下，恒星内部磁场所能达到的最大值为1017G，比由标量维里定理得到的值小一个数量级；磁场对中子系统的状态方程的影响可以忽略不计；系统的磁化率随着温度的升高而增加；在质子中子星所特有的温度范围内，比热CV随磁场变化不明显。
We investigate the effects of a magnetic field on the thermodynamics of a neutron system at finite density and temperature. Our main motivation is to deepen the understanding of the physics of a class of neutron stars known as magnetars, which exhibit extremely strong magnetic fields. Taking into account two facts, (i) the existence of a pressure anisotropy in the presence of a magnetic field and (ii) that the quantum field theory contribution to the pressure is non-negligible, we show that the maximum value that the inner magnetic field of a star can reach while being in agreement with the magnetohydrostatic equilibrium between the gravitational and matter pressures becomes 1017 G, an order of magnitude smaller than the previous value obtained through the scalar virial theorem; that the magnetic field has a negligible effect on the neutron system's equation of state; that the system's magnetic susceptibility increases with the temperature; and that the specific heat CV does not significantly change with the magnetic field in the range of temperatures characteristic of protoneutron stars.