The Labyrinth of Star Formation
The Labyrinth of Star Formation
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恒星形成的迷宫
DOI：
10.1007/978-3-319-03041-8_27
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
Bonnell I
中科院分区：
文献类型：
--
作者：
Bonnell I
我们已经进行了第一次数值模拟，以解决星星的形成过程中的亚秒差距尺度，同时也遵循星际介质（ISM）的星系尺度上的动力学。温暖的低密度ISM气体流入螺旋臂，在那里轨道拥挤产生致密云的激波形成，由外部压力暂时保持在一起。冷却使气体被压缩到足够高的密度，使局部区域在自身重力下坍塌并形成恒星。星星的形成速率与气体的局域面密度之间存在Schmidt-Kennicutt型关系，而与稠密的冷气体之间存在线性关系。冷却是星星形成的主要驱动力，而星星的形成速率决定了引力坍缩所需的冷气量。
We have performed the first numerical simulations to resolve the star formation process on sub-parsec scales, whilst also following the dynamics of the interstellar medium (ISM) on galactic scales. The warm low density ISM gas flows into the spiral arms where orbit crowding produces the shock formation of dense clouds, held together temporarily by their external pressure. Cooling allows the gas to be compressed to sufficiently high densities that local regions collapse under their own gravity and form stars. The star formation rates follow a Schmidt-Kennicutttype relation with the local surface density of gas while following a linear relation with the dense cold gas. Cooling is the primary driver of star formation and the star formation rates as it determines the amount of cold gas available for gravitational collapse.