THE STEADY-STATE WIND MODEL FOR YOUNG STELLAR CLUSTERS WITH AN EXPONENTIAL STELLAR DENSITY DISTRIBUTION
THE STEADY-STATE WIND MODEL FOR YOUNG STELLAR CLUSTERS WITH AN EXPONENTIAL STELLAR DENSITY DISTRIBUTION
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具有指数恒星密度分布的年轻星团的稳态风模型
DOI：
10.1088/0004-637x/743/2/120
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
Sergio Martínez
中科院分区：
文献类型：
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作者：
S. Silich;G. Bisnovatyi;G. Tenorio;Sergio Martínez
提出了一个恒星密度呈指数分布的年轻星团驱动的稳态球对称风的流体动力学模型。与大多数以前的计算不同的是，奇点Rsp的位置，它将内部亚音速区与外部超音速流分开，与星星集群边缘无关，但计算自洽。当辐射损失的能量可以忽略时，从亚音速流到超音速流的转变总是发生在Rsp = 4Rc处，其中Rc是恒星密度分布的特征尺度，与其他星星团参数无关。在灾难性的冷却状态下，当温度在离星星团中心很短的距离处突然下降时，情况并非如此，而从亚音速到超音速的转变发生在离星星团中心更小的距离处。详细讨论了星星团主要参数对风内部结构的影响。特别注意的是辐射冷却提供的流动的影响。的一组输入参数，这导致不同的流体动力学制度的计算结果，并比较从非辐射一维数值模拟的结果和那些从计算与均匀的恒星质量分布。
A hydrodynamic model for steady-state, spherically symmetric winds driven by young stellar clusters with an exponential stellar density distribution is presented. Unlike in most previous calculations, the position of the singular point Rsp, which separates the inner subsonic zone from the outer supersonic flow, is not associated with the star cluster edge, but calculated self-consistently. When the radiative losses of energy are negligible, the transition from the subsonic to the supersonic flow occurs always at Rsp ≈ 4Rc, where Rc is the characteristic scale for the stellar density distribution, irrespective of other star cluster parameters. This is not the case in the catastrophic cooling regime, when the temperature drops abruptly at a short distance from the star cluster center, and the transition from the subsonic to the supersonic regime occurs at a much smaller distance from the star cluster center. The impact from the major star cluster parameters to the wind inner structure is thoroughly discussed. Particular attention is paid to the effects which radiative cooling provides to the flow. The results of the calculations for a set of input parameters, which lead to different hydrodynamic regimes, are presented and compared to the results from non-radiative one-dimensional numerical simulations and to those from calculations with a homogeneous stellar mass distribution.