分子云中HII区的磁流体动力学演化：模拟方法、测试与均匀介质
天体物理学
2009-11-11 v2
摘要
我们提出了一种在磁流体动力学介质中模拟由电离辐射点源驱动的HII区演化的方法，该方法已在三维Athena MHD代码中实现。我们将使用我们的算法进行的模拟与解析解进行比较，并表明该方法通过了严格的精度和收敛性测试。这些测试揭示了电离辐射-流体动力学代码必须满足的几个条件才能重现解析解。作为我们新方法的演示，我们首次展示了HII区在磁化气体中膨胀的三维全局模拟。模拟表明，磁场抑制了垂直于磁场线方向的气体扫集，导致HII区膨胀壳前缘的密度对比度小且激波极弱。
引用
@article{arxiv.astro-ph/0606539,
title = {Magnetohydronamic Evolution of HII Regions in Molecular Clouds: Simulation Methodology, Tests, and Uniform Media},
author = {Mark R. Krumholz and James M. Stone and Thomas A. Gardiner},
journal= {arXiv preprint arXiv:astro-ph/0606539},
year = {2009}
}
备注
Accepted to ApJ. 18 pages, 19 figures, emulateapj format. Figure resolutions degraded to fit within absurdly small astroph size limits. Full resolution figures and movies of simulations available are at http://www.astro.princeton.edu/~krumholz/downloads.html . This version uses a somewhat different cooling function, but the major results are unchanged