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Particle-in-Cell Simulations and their Applications to Magnetospheres of Neutron Stars.

机译：粒子模拟及其在中子星磁层中的应用。

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摘要

Neutron stars are surrounded by dense magnetospheres with nontrivial magnetic field structure. They are sources of multi-band emission from radio waves to very high energy gamma-rays. Pulsar wind nebulae observations also show that a large number of e+/- pairs flow from the neutron star, which are produced in the magnetosphere. The structure of the magnetosphere, the mechanism of pair production and particle acceleration in the magnetosphere, and how magnetic energy is converted to kinetic energy is a complex problem that only recently has started to be addressed fully from first principles. In this dissertation I describe how I developed a numerical code tailored to study this problem. A detailed description of the code and method is given, then it is used to study the pair discharge mechanism in the magnetosphere of rotating neutron stars whose rotating axis is aligned with the magnetic axis. It was found that to form the an active magnetosphere it is necessary to have pair creation all the way towards the light cylinder. In the dissertation I classify the pulsars into two classes, and describe their differences.;The magnetospheres of magnetars are believed to be different from ordinary pulsars, in that they are sustained not by the rotation of the star, but by a twist launched from the stellar surface due to some sudden breakdown of the crust. I apply the same numerical tool to study the particle acceleration and pair creation mechanism in the twisted magnetosphere of the magnetar, showing where the gap is, and how the magnetosphere evolves over time. The magnetic twist was found to live much longer than the Alfven time of the system, and slowly dissipates through developing a cavity in the inner magnetosphere. This not only explains the long term evolution of the magnetar lightcurve after an outburst, but also explains the observed evolution hotspots on the stellar surface.
机译：中子星被具有非平凡磁场结构的致密磁层包围。它们是从无线电波到超高能伽马射线的多波段发射源。脉冲星云的观测也表明，大量e +/-对从磁层中产生的中子星流出。磁层的结构，磁层中成对产生和粒子加速的机制，以及磁能如何转换成动能是一个复杂的问题，直到最近才开始从首要原理开始全面解决。在这篇论文中，我描述了如何开发适合研究此问题的数字代码。给出了代码和方法的详细描述，然后用于研究旋转轴与磁轴对准的旋转中子星磁层中的成对放电机理。已经发现，要形成一个活跃的磁层，必须一直朝着光柱形成一对。在论文中，我将脉冲星分为两类，并描述了它们的区别。电磁星的磁层被认为与普通脉冲星不同，因为它们不是由恒星的旋转所维持，而是由恒星的旋转所维持。恒星表面由于地壳的某些突然破裂。我使用相同的数值工具来研究磁星扭曲磁层中的粒子加速和成对机制，显示间隙在哪里以及磁层随时间如何演化。发现磁扭的寿命比该系统的Alfven时间长得多，并通过在内部磁层中形成空腔而逐渐消散。这不仅解释了爆发后磁光曲线的长期演化，而且还解释了在恒星表面观察到的演化热点。

著录项

  • 作者

    Chen, Yuran Alexander.;

  • 作者单位

    Columbia University.;

  • 授予单位 Columbia University.;
  • 学科 Astrophysics.
  • 学位 Ph.D.
  • 年度 2017
  • 页码 189 p.
  • 总页数 189
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类
  • 关键词

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