超强磁场下的相对论电子  

Relativistic Electrons in Super-Strong Magnetic Fields

作　　者：宋冬灵[1] 高志福[2] 王娜[2] 杨文军[2] 彭秋和[3] 

机构地区：[1]信息工程大学理学院,河南郑州450001 [2]中国科学院新疆天文台,新疆乌鲁木齐830011 [3]南京大学天文与空间科学学院,南京210093

出　　处：《天文研究与技术》2014年第1期1-12,共12页Astronomical Research & Technology

基　　金：新疆自然科学基金面上项目(2013211A053);国家自然科学基金(11173041;11003034);973项目(2009CB824800;2012CB821800)资助

摘　　要：在以前工作的基础上,推导出超强磁场下简并的、相对论的电子压强P e的普遍表达式;讨论了电子的朗道能级量子化;探索了量子电动力学效应(QED)对中子压强占主导的理想的n-p-e气体系统的影响。主要结论包括:P e与磁场强度B、物质密度ρ及电子丰度Y e有关;磁场越强,电子压强越大;增加的压强是由高值的电子费米能引起的;在超强磁场下,磁星内部总压强是各向异性的;如果考虑到各向异性的总压强,磁星可能是一种更致密、形变后类似于椭球状的中子星;如果考虑到磁场能对状态方程的正能量的贡献,相对于普通射电脉冲星,磁星的质量可能更大些。Based on our previous work we derive a general formula for the pressure of degenerated relativisticelectron gas,P e. The formula is suitable for electron gas in super-strong magnetic fields. Subsequently,we discuss the Landau levels of electrons and investigate the Quantum Electrodynamic( QED) effects on the equations of states( EOSs) for an n-p-e ideal-gas system,the pressure of which is dominantly from neutrons. Our main conclusions are as follows.( 1) The P e is related to the magnetic induction intensity B,matter density ρ,and electron fraction Y e.( 2) The stronger the magnetic field,the higher the electron pressure.( 3) A high electron pressure could be caused by a high Fermi energy of electrons in a super-strong magnetic field.( 4) A magnetar could be a neutron star deformed by its anisotropic inner pressure to be near an oblate spheroid and to be more compact than a usual radio pulsar.( 5) Because of the positive contribution from the magnetic-field energy a magnetar can have a maximum mass larger than that of a usual radio pulsar.

关 键 词：磁星 朗道能级 超强磁场 电子费米能 电子压强 

分 类 号：P145.6[天文地球—天体物理]