中子星中简并电子气体的临界磁化

中子星内部的电子处于高度简并或完全简并的状态,电子磁矩(包括内禀磁矩和朗道反磁矩)的取向不是随机的,而是呈现出极强的磁化行为.考虑了磁化后的磁诱导方程要改写,改写后的方程添加了新的磁场生成项,更重要的改变是等效磁扩散系数变小了(顺磁情况),在临界情况(等效扩散系数等于零),磁场在磁生成项的作用下增加直到抑制机理出现,朗道反磁矩就是在这个时候变得越来越重要.磁场增加的最终结果使中子星局域磁场成为振荡的,对外看来有可能成为磁星. 关键词： 中子星 简并 磁化     

超强磁场下电子朗道能级稳定性及对电子费米能的影响

磁星是一类由磁场供能、强磁化的中子星,其内部磁场远高于电子的量子临界磁场.本文通过引入电子朗道能级的稳定性系数g_n,讨论了在磁星环境下电子的朗道能级的稳定性及其对电子费米能E_F(e)的影响;研究发现,磁场越强,电子的朗道能级越不稳定,最大的朗道能级级数n_(max)越小;朗道能级数n越大,能级稳定性系数g_n越小.根据朗道能级的稳定性系数g_n随磁场的增加而减小的要求,电子费米能表达式的磁场指数β必须是正数.通过引入Dirac-δ函数,推导出超强磁场下的简并的、相对论电子费米能的一般表达式,修正了E_F(e)的特解.新的特解给出磁场指数β=1/6;特解的适用范围ρ≥10~7g·cm~(-3),Bcr≤B≤10~(17)G.本文结果将有助于中子星内部弱相互作用过程(包括修正的URCA反应和电子俘获)和磁星磁热演化机理的研究.     

超强磁场对中子星外壳层核素56Fe,56Co,56Ni,56Mn和56Cr电子俘获过程中微子能量损失的影响

研究了超强磁场对中子星外壳层核素⁵⁶Fe,⁵⁶Co,⁵⁶Ni,⁵⁶Mn和⁵⁶Cr电子俘获过程中微子能量损失的影响.结果表明,就大部分中子星表面的磁场B<10¹³G,超强磁场对中微子能量损失率的影响很小.对于一些磁场范围为10¹³—10¹⁵G的超磁星,超强磁场可使中微子能量损失率大大降低,甚至超过5个数量级.     

基于三维磁成像的近场磁性体探测

提出一种近场条件下未知磁源的三维磁成像方法.考虑到大多数磁性体不仅受背景磁场磁化,本身也带有较强剩磁,将观测面上的磁场转换为磁场矢量异常模量,并建立目标函数进行最优化求解,以得到符合观测磁场特征的磁性体磁化模型.仿真和实验表明:此方法可有效消除剩磁对反演结果的影响,能够实现对近场多个磁源磁化率分布的成像,验证了所提方法用于探测隐含磁体位置和形状的可行性.     

欠稠密等离子体中诱发的偶次相对论谐波

在自生磁场或背景磁场的作用下,等离子体被磁化.磁化后的欠稠密等离子在超强激光的辐射下诱发相对论相干谐波辐射.由于磁场的影响,诱发的相对论相干谐波辐射中产生偶次谐波辐射.从理论上研究了这一现象,导出了谐波辐射的一般性方程,并特别研究了二次谐波辐射的有关参数 关键词： 二次谐波辐射 自生磁场 强激光 欠稠密等离子体     

外磁场中单畴反铁磁颗粒的宏观量子效应

用瞬子方法研究了外加磁场对单畴双轴反铁磁颗粒宏观量子效应的影响. 当外磁场沿易磁化方向时,简并基态中的一个能量抬高,变为亚稳态,其隧穿衰变率随外磁场增大;当外磁场沿中间磁化方向时,能级的隧穿劈裂随外磁场的变化而振荡.从而提出一种观察单畴反铁磁颗粒中宏观量子相干和隧穿现象的实验方法.     

弱相互作用费米气体的相对论顺磁性

通过考虑单粒子的相对论能量并且应用量子统计方法，研究弱磁场中弱相互作用费米气体的相对论顺磁性，求解相对论性的最可几磁化率及平均磁化率，讨论相对论效应对最可几磁化率的影响，给出相对论性的粒子数的临界值. 结果显示, 与非相对论情况比较，当 时, 相对论情况下的最可几磁化率和粒子数的临界值都没有变化. 当 时，相对论效应使系统呈现顺磁性容易，而且相对论效应增加磁化率，同时也放大了相互作用对磁化率的影响.     

超强磁场下中子星壳层的电导率和磁星环向磁场欧姆衰变

磁星是指主要由磁场提供辐射能量的一类脉冲星.部分宁静状态下的磁星X射线有热起源,对应的温度kT为0.2—0.6 keV (1 eV=1.602×10~(–19) J),这比转动供能的脉冲星的典型温度值高很多,并且可以用黑体谱来拟合.对磁星的观测和理论研究是当前脉冲星领域一个重要的热点.结合物态方程,本文首先计算了在超强磁场下壳层的电导率;从统计上研究了由于环向磁场衰变,磁场能释放率与磁星软X射线光度之间的关系.通过分类和数值拟合,所得到的新的拟合公式能较好地反映磁星软X射线光度和旋转能损率之间的关系.研究发现,对于绝大多数高X射线光度的磁星,环向磁场欧姆衰变足够提供其观测的软X射线辐射;对于低X射线光度的暂变磁星,其软X射线辐射可能来源于旋转能损率、磁层流或粒子星风.随着对磁星理论和观测研究的深入,本文模型也会得到进一步的改进,理论结果将更好地符合磁星的软X射线观测.     

弱相互作用费米气体的相对论顺磁性

通过考虑单粒子的相对论能量并且应用量子统计方法,研究弱磁场中弱相互作用费米气体的相对论顺磁性,求解相对论性的最可几磁化率及平均磁化率,讨论相对论效应对最可几磁化率的影响,给出相对论性的粒子数的临界值. 结果显示, 与非相对论情况比较,当 时, 相对论情况下的最可几磁化率和粒子数的临界值都没有变化. 当 时,相对论效应使系统呈现顺磁性容易,而且相对论效应增加磁化率,同时也放大了相互作用对磁化率的影响.     

非简并p型Hgi-xMnxTe单晶（z〉0.17）的负磁电阻机理研究

研究磁性半导体中负磁电阻产生机理对正确理解载流子与磁性离子间的sp．d磁交换作用是非常重要的．通过变温（10-300K）磁输运和变温（5-300K）磁化率实验研究了一系列不同Mn含量非简并P型Hgl-xMn。Te单晶佃〉0．17）的负磁电阻和顺磁增强效应．实验结果表明其负磁电阻与温度的关系和磁化率与温度的关系基本一致,两者都包含一个呈指数型变化的温度函数exp（-K／T）．根据磁性半导体的杂质能级理论,非简并P型H譬1-xMnxTe单晶在低磁场范围内出现负磁电阻效应的主要物理机理为外磁场的磁化效应使得受主杂质或受主型束缚磁极化子的有效电离能减小．     

Thermodynamic functions of a nonrelativistic degenerate neutron gas in a magnetic field

The Fermi energy, partial concentrations of polarized neutrons, pressure, and volume energy density of a degenerate nonrelativistic neutron gas in a magnetic field are calculated using numerical methods taking into account the anomalous magnetic moment of a neutron. The results of calculations are a generalization of relations underlying the Oppenheimer-Volkov model of a neutron star to the case of an applied magnetic field. An ultrastrong (up to 10¹⁷ G) magnetic field changes the pressure and internal energy of the star and affects it static configuration and evolution. It is shown that a degenerate neutron gas in ultrastrong and weak magnetic fields is paramagnetic; the corresponding values of magnetic susceptibility differ by a factor on the order of unity. The possibility of experimentally verifying the results from analysis of pulsar-emitted radiation is discussed.     

THE POSSIBLE ORIGIN OF STRCNG MAGNETIC FIELD OF NEUTRON STAR:FERROMAGNETIC STATE

The magnetic susceptibility of neutron matter was calculated by means of Owen's LOCV method. The results showed that a transition to a ferromagnetic state can exist for HJ, IY and M-S potentials, but there is no transition for Reid soft-core potential .By analyses, we concluded that the ferromagnetic state is a possible origin of strong magnetic field within the neutron star. We also considered an influence of the ferromagnetic state on the mass, radius and moment of inertia of the neutron star.Finally we discussed the effect of magnetization on physical state in the neutron star.     

On the neutronization radius of magnetic neutron stars: The field and temperature dependences of the chemical potential and minimum number density of a degenerate magnetized electron gas

The temperature and field dependences of the chemical potential and the field dependence of the Fermi energy for a degenerate relativistic electron gas in a magnetic field have been analyzed by numerical and analytical methods. An analytical expression has been derived for the dependence of the minimum electron number density and the corresponding neutronization radius on the magnetic field strength in a collapsing star upon its subsequent transformation into a neutron one. We believe that a similar relation also holds for the equilibrium neutron star radius. Our results refine the conclusions reached previously [1] in the case of a nonzero temperature and the influence of the star??s proton component on the neutronization process as well as confirm and generalize them in terms of a significant (by an order of magnitude or severalfold) decrease in the equilibrium radius of a neutron star in a superstrong (10¹⁴?C10¹⁷ G) magnetic field compared to the case where there is no such field. We point out that there may exist a separate class of stellar objects??very small magnetar neutron stars that we propose to name ??minimagnetars??. We hypothesize that they can be the final evolutionary stage of stars before their collapse into a black hole.     

Magnetism of a relativistic degenerate electron gas in a strong magnetic field

The magnetization and magnetic susceptibility of a degenerate electron gas in a strong magnetic field in which electrons are located on the ground Landau level and the electron gas has the properties of a nonlinear paramagnet have been calculated. The paradoxical properties of the electron gas under these conditions??a decrease in the magnetization with the field and an increase in the magnetization with the temperature??have been revealed. It has been shown that matter under the corresponding conditions of neutron stars is a paramagnet with a magnetic susceptibility of ?? ?? 0.001.     

Microscopic calculation of the magnetic field of neutron stars

Based on the Dirac equation describing an electron moving in a uniform and cylindrically symmetric magnetic field which may be the result of the self-consistent mean field of the electrons themselves in a neutron star, we have obtained the eigen solutions and the orbital magnetic moments of electrons in which each eigen orbital can be calculated. From the eigen energy spectrum we find that the lowest energy level is the highly degenerate orbitals with the quantum numbers pZ=0, n=0, and m≥0. At the ground state, the electrons fill the lowest eigen states to form many Landau magnetic cells and each cell is a circular disk with the radius λfree and the thickness λe, where λfree is the electron mean free path determined by Coulomb cross section and electron density and λe is the electron Compton wavelength. The magnetic moment of each cell and the number of cells in the neutron star are calculated, from which the total magnetic moment and magnetic field of the neutron star can be calculated. The results are compared with the observational data and the agreement is reasonable.     

Influence of the nuclear equation of state on the hadron-quark phase transition in neutron stars

We study the hadron-quark phase transition in the interior of neutron stars, and examine the influence of the nuclear equation of state on the phase transition and neutron star properties. The relativistic mean field theory with several parameter sets is used to construct the nuclear equation of state, while the     

Electromagnetic activity of a pulsating paramagnetic neutron star

The fact that neutron star matter possesses the capability of maintaining a highly intense magnetic field has been and still is among the most debatable issues in pulsar astrophysics. Over the years, there were several independent suggestions that the dominant source of pulsar magnetism is either the field-induced or the spontaneous magnetic polarization of the baryon material. The Pauli paramagnetism of degenerate neutron matter is one of the plausible and comprehensive mechanisms of the magnetic ordering of neutron magnetic moments, promoted by a seed magnetic field inherited by the neutron star from a massive progenitor and amplified by its implosive contraction due to the magnetic flux conservation. Adhering to this attitude and based on the equations of magnetoelastic dynamics underlying continuum mechanics of single-axis magnetic insulators, we investigate electrodynamics of a paramagnetic neutron star undergoing nonradial pulsations. We show that the suggested approach regains a recent finding of Akhiezer et al. [1] that the spin-polarized neutron matter can transmit perturbations by low-frequency transverse magnetoelastic waves. We found that nonradial torsional magnetoelastic pulsations of a paramagnetic neutron star can serve as a powerful generator of a highly intense electric field producing the magnetospheric polarization charge whose acceleration along the open magnetic field lines leads to the synchrotron and curvature radiation. Analytic and numerical estimates for periods of non-radial torsional magnetoelastic modes are presented and are followed by a discussion of their possible manifestation in currently monitored activity of pulsars and magnetars.     

Quark stars: features and findings

Under extreme conditions of temperature and/or density, quarks and gluons are expected to undergo a deconfinement phase transition. While this is an ephemeral phenomenon at the ultra-relativistic heavy-ion collider (BNL-RHIC), quark matter may exist naturally in the dense interior of neutron stars. Here, we present an appraisal of the possible phase structure of dense quark matter inside neutron stars, and the likelihood of its existence given the current status of neutron star observations. We conclude that quark matter inside neutron stars cannot be dismissed as a possibility, although recent observational evidence rules out most soft equations of state. PACS 97.60.Jd; 26.60.+c