超强磁场下简并电子气体的磁化

致密天体（白矮星和中子星）内部的电子气体是简并的费米系统，它们的零点费米动能远大于热运动动能。根据零点费米能与电子静止能的比较可区分为非相对论和相对论两种情况,按电子拉莫尔轨道动能与零点费米能的比较又可区分为强和超强两种外磁场作用情况。本文研究了电子费米系统在超强磁场作用下的磁化问题,发现在非相对论和相对论两种情况中的磁化都呈现出de Haas-van Alphen 震荡效应,但微分磁化率难以大于临界值1,说明在超强磁场下的电子气体难以发生Condon磁相变,只有当电子占据刚好填满第一朗道量子能级时,微分磁化率才能大于一。

Magnetization of Degenerate Electron Gas Under Super-strong Magnetic Field

The dense electron gases inside condensed ob ject （including white dwarf and neutron star） are Fermi systems with high degenerate.The Fermi energy at zero temperature is more larger than thermo kinetic energy.According to the difference between the Fermi energy and the rest energy of electron,electron gas is considered as either no-relativistic or relativistic.The difference between the rest energy and the cyclotron energy can distinguish the magnetic field which is either strong or super-strong.In this paper,we study the magnetization of degenerate electron gas under super-strong magnetic field.We found that the magnetiza-tion under super-strong magnetic field is oscillated just like de Haas-van Alphen oscillation.The differential susceptibility is smaller than 1 and the Condon magnetic phase transition does not take place except at the condition when electrons fill up the first Landau level.