星系群卫星日冕气体的去除和混合：冷却星系群内气体
Removal and mixing of the coronal gas from satellites in galaxy groups: cooling the intragoup gas
摘要：
在星系团、星系群和大质量星系周围存在着一个扩展的热气日冕，这一点已被观测证据所证实，并被当前的星系形成理论所预言。当一个小星系与一个大星系碰撞时，它们的日冕首先相互作用，产生扰动，将气体从较小的系统中移除，并将其沉降到较大系统的日冕中。对于一个银河系大小的星系合并成一个低质量的群体，冲压压力剥离和开尔文-亥姆霍兹不稳定性是最相关的这些扰动。我们认为，由后者产生的湍流混合材料的两个日冕在轨道卫星的尾流中创建一个“暖相”的混合物与冷却时间的一个因素的几个短于周围的组内气体。我们得出这一结论，使用解析估计，以及绝热和耗散的高分辨率数值模拟的球形日冕的消融过程中的一个恒定的速度风均匀的密度和温度。虽然这是一个初步的分析，我们的研究结果是有希望的，我们推测，混合物可能会引发原位恒星形成和/或吸积到中央星系作为一个冷的气体流导致在星系群和星系团的恒星形成的新模式。
英文摘要：
The existence of an extended hot gaseous corona surrounding clusters, groups and massive galaxies is well established by observational evidence and predicted by current theories of galaxy formation. When a small galaxy collides with a larger one, their coronae are the first to interact, producing disturbances that remove gas from the smaller system and settle it into the corona of the larger one. For a Milky-Way-size galaxy merging into a low-mass group, ram pressure stripping and the Kelvin-Helmholtz instability are the most relevant of these disturbances. We argue that the turbulence generated by the latter mixes the material of both coronae in the wake of the orbiting satellite creating a "warm phase" mixture with a cooling time a factor of several shorter than that of the ambient intragroup gas. We reach this conclusion using analytic estimates, as well as adiabatic and dissipative high resolution numerical simulations of a spherical corona subject to the ablation process of a constant velocity wind with uniform density and temperature. Although this is a preliminary analysis, our results are promising and we speculate that the mixture could potentially trigger in situ star formation and/or be accreted into the central galaxy as a cold gas flow resulting in a new mode of star formation in galaxy groups and clusters.
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