The magnetospheric plasma distribution in the vicinity of a pulsar at various inclination angles is investigated using a new relativistic, parallel 3D Particle-In-Cell (PIC) code DYMPHNA3D. DYMPHNA3D uses a superposition of the electromagnetic fields associated with a rotating magnetised conducting sphere in a vacuum (the pulsar fields) and the electromagnetic fields due to the presence of the magnetospheric plasma surrounding the pulsar (the plasma fields), as the total fields. The plasma is moved self-consistently through the magnetosphere using the PIC methodology. Our initial simulation results are presented here. These show similar solutions to those obtained from previous numerical simulations, which show the fundamental plasma distribution in the vicinity of an aligned rotating neutron star to consist of two polar domes and an equatorial torus of trapped non-neutral plasma of opposite sign. The aligned case being the case in which the inclination angle between the magnetic dipole moment and the rotation axis of the star is zero. Furthermore, our code allows for off-axis simulations and we have found that this plasma distribution collapses into a Quad-Lobe charge-separated non-neutral magnetospheric plasma distribution in the case of an orthogonal rotator, i.e., the case in which the magnetic dipole moment is oriented at right angles to the rotation axis of the neutron star, with the plasma remaining trapped close to the stellar surface by the force-free surfaces. We find that if initialised with a Goldreich-Julian type distribution, the system is seen to collapse rapidly into these stable Dome-Torus structures.
A periodically active pulsar giving insight into magnetospheric physics
PSR B1931+24（J1933+2421）是一颗孤立的射电脉冲星，活跃期为5-10天。然而，无线电发射在不到10秒的时间内关闭，并在接下来的25-35天内无法检测到，然后再次打开。这种模式准周期性地重复。这种行为的起源尚不清楚。更值得注意的是，脉冲星的自转速度在开启时比关闭时快50%。这表明当脉冲星开启时，磁层电流大量增加，证明脉冲星风在脉冲星自旋下降中起着重要作用。这使我们能够，第一次，估计电流在脉冲星磁层发生无线电发射。
Effects of Rotation and Relativistic Charge Flow on Pulsar Magnetospheric Structure
提出了一个中子星（NS）磁层开磁力线区的三维解析模型。我们构建了一个显式的解析解任意的磁层旋转（旋转和磁轴之间的角度），将磁层旋转的影响，相对论流动的电荷（如初级电子束）沿开放场线，和E X B漂移这些费用。我们的解决方案采用了空间电荷限制的纵向电流计算的电动模型的Alummov和Tsygan（1992年），是有效的非常高的高度接近轻圆柱体。我们假设在磁层的最内层，NS磁场可以很好地表示为静态磁偶极子位形。在高海拔的开放磁场线显着偏离那些静态偶极子，并往往集中成一个圆柱形束，扫回的方向相反的旋转，也向旋转赤道弯曲。我们简要地讨论了我们的研究的自旋动力的光子晶体的一些启示。
