在超强磁场中修正的相对论电子压强  

Modified pressure of relativistic electrons in a superhigh magnetic field

作　　者：董爱军 高志福[2] 杨晓峰[2] 王娜[2] 刘畅 彭秋和[3] Dong Ai-Jun;Gao Zhi-Fu;Yang Xiao-Feng;Wang Na;Liu Chang;Peng Qiu-He(School of Physics and Electronic Science,Guizhou Normal University,Guiyang 550001,China;Xinjiang Astronomical Observatory,Chinese Academy of Sciences,Urumqi 830011,China;School of Astronomy&Space Science,Nanjing University,Nanjing 210000,China;Guizhou Provincial Key Laboratory of Radio Data Processing,Guiyang 550001,China)

机构地区：[1]贵州师范大学物理与电子科学学院,贵阳550001 [2]中国科学院新疆天文台,乌鲁木齐830011 [3]南京大学天文与空间科学学院,南京210000 [4]贵州省射电天文数据处理重点实验室,贵阳550001

出　　处：《物理学报》2023年第3期37-51,共15页Acta Physica Sinica

基　　金：国家自然科学基金(批准号:12041304,U1831120);新疆维吾尔自治区自然科学基金(批准号:2022D01A155);贵州省科技计划(批准号:[2019]1241,KY(2020)003);中科院高层次人才计划择优支持项目(批准号:[2019]085)资助的课题。

摘　　要：当前脉冲星领域一个重要的研究热点是磁星.本文在朱翠等(Zhu C,Gao Z F,Li X D,Wang N,Yuan J P,Peng Q H 2016 Mod.Phys.Lett.311650070)工作的基础上,重新研究了磁星超强磁场下(B>>B_(cr),B_(cr)是电子的.量子临界磁场)电子朗道能级的稳定性及其对电子压强的影响.首先,对弱磁场极限下(B<<B_(cr))中子星内部电子压强进行必要的回顾;然后,通过引入电子朗道能级稳定性系数g_(v)和Dirac-δ函数,推导出在超强磁场下修正的相对论电子压强P_(e)的表达式,给出表达式适用条件:物质密度P≥10^(7)g·cm^(-3).和B_(cr)≤B<10^(17)G(1 G=10^(-4)T).超强磁场通过修正相对论电子的相空间,提高了电子数密度n_(e),而n_(e)的增加意味着Pe的增加.利用修正的电子压强表达式,讨论了超强磁场下费米子自旋极化现象、电子磁化现象以及超强磁场对物态方程的修正.最后,本文的结果与其他类似工作进行对比,并对未来的工作进行展望.本文的研究将为磁星以及强磁化白矮星的物态方程和热演化的探索提供极有价值的参考,将为普通射电脉冲星等离子磁层数值模拟、高磁场脉冲星辐射机制等相关研究提供有用的信息.Magnetar is a kind of pulsar powered by magnetic field energy.The study of magnetars is an important hotspot in the field of pulsars.In this paper,according to the work of Zhu Cui,et al.(Zhu C,Gao Z F,Li X D,Wang N,Yuan J P,Peng Q H 2016 Mod.Phys.Lett.A 311650070),we reinvestigate the Landau-level stability of electrons in a super high magnetic field(SMF),B>>B_(cr)(B_(cr)is a quantum critical magnetic field with a value of 4.414×10^(13)G),and its influence on the pressure of electrons in magnetar.First,we briefly review the pressure of electrons in neutron star(NS)with a weak-magnetic field limit(B<<B_(cr)).Then,we introduce an electron Landau level stability coefficient gvand a Dirac-δfunction to deduce a modified pressure formula for the degenerate and relativistic electrons in an SMF in an application range of matter densityρ≥10^(7) g·cm^(-3)and B_(cr)<<B<10^(17)G.By modifying the phase space of relativistic electrons,the SMF can enhance the electron number density ne,and reduce the maximum of electron Landau level number vmax,which results in a redistribution of electrons.As B increases,more and more electrons will occupy higher Landau levels,and the electron Landau level stability coefficient gvwill decrease with the augment of Landau energy-level number v.By modifying the phase space of relativistic electrons,the electron number density neincreases with the MF strength increasing,leading the electron pressure Peto increase.Utilizing the modified expression of electron pressure,we discuss the phenomena of Fermion spin polarization and electron magnetization in the SMF,and the modification of the equation of state by the SMF.We calculate the baryon number density,magnetization pressure,and the difference between pressures in the direction parallel to and perpendicular to the magnetic field in the frame of the relativistic mean field model.Moreover,we find that the pressure anisotropy due to the strong magnetic field is very small and can be ignored in the present model.We compare our results with the re

关 键 词：超强磁场 朗道能级 磁星 磁化 

分 类 号：O572.322[理学—粒子物理与原子核物理]