星际介质中湍流结构形成及其与观测之间的联系
摘要
本文综述了关于湍流星际介质(ISM)的数值模拟所得的最新结果，特别是关于湍流云的本质与形成、用于比较模拟中结构与观测之间的方法，以及三维结构投射到二维上的影响。作为湍流密度波动形成的云，可能并非受热压约束，相反，其形态可能由大尺度速度场决定。此外，这些云的寿命可能比通常所认为的要短，因为大尺度湍流模式具有较大的相关速度，而这些速度超过了云内部速度分布。结构表征算法已开始区分最适合特定观测的模拟，并开启了若干新问题，如观察到的线宽-尺度关系以及信道图中结构与密度场和速度场真实空间分布之间的关系。速度场似乎在强度信道图中占据主导地位，至少在密度场的功率谱足够陡峭的情况下如此。 Furthermore, the selection of scattered fluid parcels along the line of sight (LOS) by their LOS-velocity inherent to the construction of spectroscopic data may introduce spurious small-scale structure in high spectral resolution channel maps. Furthermore, the selection of scattered fluid parcels along the line of sight (LOS) by their LOS-velocity inherent to the construction of spectroscopic data may introduce spurious small-scale structure in high spectral resolution channel maps.
引用
@article{arxiv.astro-ph/9908074,
title = {Turbulent Formation of Interstellar Structures and the Connection Between Simulations and Observations},
author = {Enrique Vázquez-Semadeni},
journal= {arXiv preprint arXiv:astro-ph/9908074},
year = {2018}
}
备注
15 pages, no figures. To appear in the Proceedings of "The Chaotic Universe", Roma/Pescara, Italy, 1-5 Feb. 1999, eds. V. Gurzadyan and L. Bertone. Uses included .cls file