Three-Dimensional Simulation of Molecular Cloud Formation
Three-Dimensional Simulation of Molecular Cloud Formation
复制标题
分子云形成的三维模拟
DOI：
10.1007/978-3-319-03041-8_30
复制
发表时间：
2014
期刊：
影响因子：
--
通讯作者：
Tsuyoshi
中科院分区：
文献类型：
--
作者：
Inoue;Tsuyoshi
Using three-dimensional magnetohydrodynamics simulation with the effects of radiative cooling/heating, chemical reactions, and thermal conduction, we investigate the formation of molecular cloud in the multi-phase interstellar medium. As suggested by recent observations, we consider shock compression of HI clouds as a triggering mechanism of the molecular cloud formation. The simulation shows that the initial HI medium is compressed and piled up behind the shock waves induced by the accretion flows. The post shock region is composed of dense cold clumps (T< 100 K) and diffuse thermally unstable gas (T> 1, 000 K), which are spatially well mixed owing to the supersonic turbulence. In the molecular cloud, clumps evolve with time by condensation accretion of the diffuse gas and collisional coalescence of the clumps. Statistics of the clumps suggest that the typical initial condition of molecular cloud core is magnetically super-critical.
