We present a suite of three-dimensional, high-resolution hydrodynamic simulations that follow the evolution of a massive (10^7 M_sun) pressure confined, star-forming neutral gas cloud moving through a hot intra-cluster medium (ICM). The main goal of the analysis is to get theoretical insight into the lifetimes and evolution of stellar systems like the recently discovered star-forming cloud SECCO~1 in the Virgo cluster of galaxies, but it may be of general interest for the study of the star-forming gas clumps that are observed in the tails of ram pressure stripped galaxies. Building upon a previous, simple simulation, we explored the effect of different relative velocity of the cloud and larger temperature of the ICM, as well as the effect of the cloud self-gravity. Moreover, we performed a simulation including star-formation and stellar feedback, allowing for a first time a direct comparison with the observed properties of the stars in the system. The survivability of the cold gas in the simulated clouds is granted on timescales of the order of 1 Gyr, with final cold gas fractions generally $>0.75$. In all cases, the simulated systems end up, after 1 Gyr of evolution, as symmetric clouds in pressure equilibrium with the external hot gas. We also confirm that gravity played a negligible role at the largest scales on the evolution of the clouds. In our simulation with star formation, star formation begins immediately, it peaks at the earliest times and decreases monotonically with time. Inhomogeneous supernova explosions are the cause of an asymmetric shape of the gas cloud, facilitating the development of instabilities and the decrease of the cold gas fraction.

中文翻译：

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室女座星团中孤立的恒星形成气体云的流体动力学模拟

我们展示了一套三维、高分辨率的流体动力学模拟，这些模拟遵循一个巨大的 (10^7 M_sun) 压力限制、恒星形成的中性气体云穿过热的簇内介质 (ICM) 的演变。分析的主要目标是从理论上深入了解恒星系统的寿命和演化，例如最近在室女座星系团中发现的恒星形成云 SECCO~1，但它可能对恒星的研究具有普遍意义。 -在撞击压力剥离的星系的尾部观察到的形成气体团块。在之前的简单模拟的基础上，我们探索了云的不同相对速度和 ICM 较大温度的影响，以及云自重的影响。此外，我们进行了包括恒星形成和恒星反馈在内的模拟，首次允许与系统中恒星的观测特性进行直接比较。模拟云中冷气的生存能力在 1 Gyr 量级的时间尺度上被授予，最终冷气部分通常 $>0.75$。在所有情况下，模拟系统在 1 Gyr 演化后最终成为与外部热气体压力平衡的对称云。我们还证实，重力在云演化的最大尺度上所起的作用可以忽略不计。在我们对恒星形成的模拟中，恒星形成立即开始，它在最早的时间达到峰值，并随时间单调减少。不均匀的超新星爆炸是气体云形状不对称的原因，促进了不稳定性的发展和冷气体比例的减少。