ROTATING NEUTRON STAR MODELS WITH MAGNETIC FIELD
ROTATING NEUTRON STAR MODELS WITH MAGNETIC FIELD
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发表时间：
1995-03
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通讯作者：
M. Bocquet;S. Bonazzola;E. Gourgoulhon;J. Novak
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作者：
M. Bocquet;S. Bonazzola;E. Gourgoulhon;J. Novak
我们提出了第一个数值解的耦合Einstein-Maxwell方程描述快速旋转的中子星赋予一个磁场。这些解是完全相对论性和自洽的，所有的电磁场对星星平衡的影响（洛伦兹力，电磁应力-能量产生的时空曲率）都被考虑在内。磁场是轴对称和极向的。采用了五个稠密物质状态方程。偏微分方程系统集成的伪谱方法。给出了数字编码通过的各种测试。然后研究了磁场对中子星结构的影响，特别是通过比较具有相同重子数的磁化和非磁化组态。磁场引起的星星的变形只有在B值很大（B>10^{10} T）时才重要。最大质量以及最大旋转速度被发现与磁场的增加。最大允许极向磁场是10^{14} T（10^{18} G）的量级，并且当磁压力与星星中心的流体压力相当时达到。对于这样的值，中子星的最大质量被发现增加了13%至29%（取决于状态方程）相对于非磁化恒星的最大质量。
We present the first numerical solutions of the coupled Einstein-Maxwell equations describing rapidly rotating neutron stars endowed with a magnetic field. These solutions are fully relativistic and self-consistent, all the effects of the electromagnetic field on the star's equilibrium (Lorentz force, spacetime curvature generated by the electromagnetic stress-energy) being taken into account. The magnetic field is axisymmetric and poloidal. Five dense matter equations of state are employed. The partial differential equation system is integrated by means of a pseudo-spectral method. Various tests passed by the numerical code are presented. The effects of the magnetic field on neutron stars structure are then investigated, especially by comparing magnetized and non-magnetized configurations with the same baryon number. The deformation of the star induced by the magnetic field is important only for huge values of B (B>10^{10} T). The maximum mass as well as the maximum rotational velocity are found to increase with the magnetic field. The maximum allowable poloidal magnetic field is of the order of 10^{14} T (10^{18} G) and is reached when the magnetic pressure is comparable to the fluid pressure at the centre of the star. For such values, the maximum mass of neutron stars is found to increase by 13 to 29 % (depending upon the EOS) with respect to the maximum mass of non-magnetized stars.