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Equilibrium of Rotating Strongly Magnetized Star and Abrupt Energy Release

旋转强磁化恒星的平衡与能量突变

基本信息

批准号：
16540256
负责人：
KOJIMA Yasufumi
金额：
$ 2.48万
依托单位：
Hiroshima University
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
2004
资助国家：
日本
起止时间：
2004 至 2007
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16540256/
关键词：
neutron star relativity plasma MHD

项目摘要

The magnetic fields and stellar rotation are very important for the burst on relativistic stars. The purpose of this research project is to clarify the electromagnetic field structure around the strongly magnetized stars and to clarify the propagation and transmission of energy from the interior of the star to external magnetosphere, where plasma may be accelerated by the reconnection of magnetic field or some other mechanism and the energy is eventually transformed to radiation. Propagation and the transmission of Alfven waves in strongly magnetized stars are examined. It is found that the displacement currents and stellar rotation are complicatedly coupled, and hence are very important in magnetically dominated regime.A new numerical code to solve electromagnetic fields and plasma motion has developed. Axially symmetry and two component fluids are assumed. This code is different from MHD approximation, and can be used even for electrically dominated case. The preliminary results are obtained and the numerical code is now applied to realistic case: construction of pulsar magnetosphere and a model of gamma ray repeaters.Some new results are published for related topics for neutron stars. They are magnetic field decay, constraints on the equation of states for neutron star interior from some observations, resonant pulsation due to external gravitational waves, gyro motion in tidal gravity, and nonlinear growth of bar instability of rotating stars.

磁场和恒星自转对相对论性恒星的爆发有着重要的影响。该研究项目的目的是阐明强磁化恒星周围的电磁场结构，并阐明能量从星星内部向外部磁层的传播和传输，其中等离子体可能因磁场重联或其他某种机制而加速，能量最终转化为辐射。研究了阿尔芬波在强磁化恒星中的传播和透射。结果表明，位移电流与恒星自转之间存在着复杂的耦合关系，在磁主导区中具有重要的作用.轴对称和两个组件的流体假设。该程序与MHD近似不同，甚至可以用于电占优的情况。得到了初步的结果，并将数值计算程序应用于脉冲星磁层的构造和γ射线中继器的模型中，在中子星的相关课题中也得到了一些新的结果。它们是磁场衰减、观测到的中子星星内部状态方程的约束、外部引力波引起的共振脉动、潮汐引力中的陀螺运动以及旋转恒星棒不稳定性的非线性增长。