Ram pressure stripping can remove gas from satellite galaxies in clusters via a direct interaction between the intracluster medium (ICM) and the interstellar medium. This interaction is generally thought of as a contact force per area; however, we point out that these gases must interact in a hydrodynamic fashion and argue that this will lead to the mixing of the galactic gas with the ICM wind. We develop an analytic framework for how mixing is related to the acceleration of stripped gas from a satellite galaxy. We then test this model using three “wind-tunnel” simulations of Milky Way–like galaxies interacting with a moving ICM and find excellent agreement with predictions using the analytic framework. Focusing on the dense clumps in the stripped tails, we find that they are nearly uniformly mixed with the ICM, indicating that all gas in the tail mixes with the surroundings and dense clumps are not separate entities to be modeled differently than diffuse gas. We find that while mixing drives the acceleration of stripped gas, the density and velocity of the surrounding wind will determine whether the mixing results in the heating of stripped gas into the ICM or the cooling of the ICM into dense clouds.

冲压压力剥离可以通过星团内介质 (ICM) 和星际介质之间的直接相互作用从星团中的卫星星系中去除气体。这种相互作用通常被认为是单位面积的接触力；然而，我们指出这些气体必须以流体动力学方式相互作用，并认为这将导致银河气体与 ICM 风混合。我们开发了一个关于混合如何与卫星星系剥离气体加速相关的分析框架。然后，我们使用银河系类星系与移动 ICM 相互作用的三个“风洞”模拟来测试该模型，并发现与使用分析框架的预测非常吻合。关注剥离尾部的密集团块，我们发现它们几乎均匀地与 ICM 混合，表明尾部的所有气体都与周围环境混合，并且密集的团块不是单独的实体，与扩散气体不同地建模。我们发现，在混合驱动汽提气体加速的同时，周围风的密度和速度将决定混合是导致汽提气体加热进入 ICM 还是导致 ICM 冷却成为密云。