PAIR-STARVED PULSAR MAGNETOSPHERES
PAIR-STARVED PULSAR MAGNETOSPHERES
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DOI：
10.1088/0004-637x/692/1/140
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发表时间：
2008-10
期刊：
影响因子：
--
通讯作者：
A. Muslimov;A. K. Harding
中科院分区：
文献类型：
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作者：
A. Muslimov;A. K. Harding
本文提出了一个简单的解析模型，用于描述旋转中子星星（NS）的最内层（正则半径为λ c/Ω的光柱（LC）内）的开磁力线结构，其中NS的自旋和磁轴之间具有任意角度，且有相对论性的带电粒子（电子/正电子）流出.我们提出了磁场和电流的麦克斯韦方程组的自洽解决方案，在对饥饿的制度，电子-正电子等离子体的密度以上产生的脉冲星极冠是不足以完全屏蔽加速电场，从而建立E · B = 0的条件以上的对形成前锋到非常高的高度内的LC。该模型可以为发展全球成对饥饿脉冲星磁层精细模型提供理论框架。
We propose a simple analytic model for the innermost (within the light cylinder (LC) of canonical radius ∼c/Ω) structure of open-magnetic-field lines of a rotating neutron star (NS) with relativistic outflow of charged particles (electrons/positrons) and an arbitrary angle between the NS spin and magnetic axes. We present the self-consistent solution of Maxwell's equations for the magnetic field and electric current in the pair-starved regime where the density of electron–positron plasma generated above the pulsar polar cap is not sufficient to completely screen the accelerating electric field and thus establish the E · B = 0 condition above the pair-formation front up to the very high altitudes within the LC. The proposed model may provide a theoretical framework for developing the refined model of the global pair-starved pulsar magnetosphere.