大质量致密巨星团M82-A1的压力约束风
The pressure confined wind of the massive and compact superstar cluster M82-A1
摘要：
这里所观察到的参数的年轻的超级巨星团M82-A1和它的相关的紧凑的HII区域显示，通过辐射冷却，一个低的加热效率或立即损失的大部分能量插入恒星风和超新星在早期的集群演化。这意味着一个双峰流体动力学的解决方案，这导致到ISM的质量沉积速率降低，流出速度大大降低。此外，为了与M82-A1相关的HII区的观测参数相匹配，这里所得到的星团风应该被高压星际介质所限制。通过解析方法推导出团风参数以及反向激波的位置、冷却长度和HII外区的半径。所有这些属性，然后确认与半解析积分的流动方程，这也为我们提供了运行的流体动力学变量作为半径的函数。的影响的结果进行了讨论，并扩展到其他大规模的和年轻的超巨星团所包围的一个紧凑的HII区域。
英文摘要：
The observed parameters of the young superstar cluster M82-A1 and its associated compact HII region are here shown to indicate a low heating efficiency or immediate loss, through radiative cooling, of a large fraction of the energy inserted by stellar winds and supernovae during the early evolution of the cluster. This implies a bimodal hydrodynamic solution which leads to a reduced mass deposition rate into the ISM, with a much reduced outflow velocity. Furthermore, to match the observed parameters of the HII region associated to M82-A1, the resultant star cluster wind is here shown to ought to be confined by a high pressure interstellar medium. The cluster wind parameters, as well as the location of the reverse shock, its cooling length and the radius of the standing outer HII region are derived analytically. All of these properties are then confirmed with a semi-analytical integration of the flow equations, which provides us also with the run of the hydrodynamic variables as a function of radius. The impact of the results is discussed and extended to other massive and young superstar clusters surrounded by a compact HII region.
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