We use a cosmological chemodynamical simulation to study how the group environment impacts the star formation (SF) properties of disk galaxies. The simulated group has a total mass of M ～ 8 × 10 ~ (12) solar mass and a total X-ray luminosity of L_x ～ 10~(41) erg s~(-1). Our simulation suggests that ram pressure is not sufficient in this group to remove the cold disk gas from a V_(rot) ～ 150 km s~(-1) galaxy. However, the majority of the hot gas in the galaxy is stripped over a timescale of approximately 1 Gyr. Since the cooling of the hot-gas component provides a source for new cold gas, the stripping of the hot component effectively cuts off the supply of cold gas. This in turn leads to a quenching of SF. The galaxy maintains the disk component after the cold gas is consumed, which may lead to a galaxy similar to an SO. Our self-consistent simulation suggests that this strangulation mechanism works even in low-mass groups, providing an explanation for the lower SF rates in group galaxies relative to galaxies in the field.
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机译：我们使用宇宙化学动力学模拟来研究群环境如何影响盘状星系的恒星形成（SF）特性。模拟组的总质量为M〜8×10〜（12）太阳质量，总X射线发光度为L_x〜10〜（41）erg s〜（-1）。我们的模拟表明，该组中的冲压压力不足以从V_（rot）〜150 km s〜（-1）星系中除去冷盘气体。但是，银河系中的大部分热气体在大约1 Gyr的时间范围内被汽提。由于热气组分的冷却为新的冷气提供了来源，因此热组分的汽提有效地切断了冷气的供应。这进而导致SF的淬灭。消耗冷气体后，星系会保留磁盘组件，这可能会导致类似于SO的星系。我们的自洽模拟表明，这种扼杀机制甚至适用于低质量群，这也解释了相对于野外星系，群星系的SF率较低。
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