论文标题
3D相对论的MHD模拟
3D Relativistic MHD Simulations of Pulsar Bow Shock Nebulae
论文作者
论文摘要
脉冲星的父snR直接与产生所谓的弓箭脉冲星风星云（Heliospherivistivics iperivistion等当量）直接与ISM相互作用。这些从无线电到X射线直接观察到，也发现与TEV Halos有关，并具有各种形态。他们提供了一个独特的环境，可以通过与周围环境介质进行建模，以与规范杂物不同/互补的方式来研究脉冲星风。与暗物质相比，这些系统还被认为是AMS和Pamela检测到的正电子过剩的可能起源。我将从3D相对论的MHD模拟此类星云中提出结果。在这些模拟的顶部，我们计算了预期的发射特征，高能粒子逃逸的特性，电流板在引导宇宙射线中的作用，湍流和磁扩增的水平以及它们如何依赖风结构和磁性。
Pulsars out of their parent SNR directly interact with the ISM producing so called Bow-Shock Pulsar Wind Nebulae, the relativistic equivalents of the heliosphere/heliotail system. These have been directly observed from Radio to X-ray, and are found also associated to TeV halos, with a large variety of morphologies. They offer a unique environment where the pulsar wind can be studied by modelling its interaction with the surrounding ambient medium, in a fashion that is different/complementary from the canonical Plerions. These systems have also been suggested as the possible origin of the positron excess detected by AMS and PAMELA, in contrast to dark matter. I will present results from 3D Relativistic MHD simulations of such nebulae. On top of these simulations we computed the expected emission signatures, the properties of high energy particle escape, the role of current sheets in channeling cosmic rays, the level of turbulence and magnetic amplification, and how they depend on the wind structure and magnetisation.
