时间中的一个时刻-模拟太阳系中的恒星形成
One moment in time - modeling star formation in the Antennae
摘要：
我们提出了一个新的高分辨率的N体/SPH模拟遇到的两个富含气体的盘星系密切匹配的相互作用的星系（NGC 4038/39）的形态和运动学。模拟包括辐射冷却、恒星形成和SNII的反馈。大尺度的形态学和运动学是由祖先盘的内部结构和轨道决定的。中心区域的性质，特别是在重叠区域的星爆，只在第二次相遇后约2000万年的非常短的时间间隔内与观测结果相匹配。这表明，在第二次碰撞后约4000万年和最后一次碰撞前约5000万年，银河系处于一个特殊的阶段。这是模拟中唯一的阶段，当核之间的富含气体的重叠区域形成时，伴随着增强的恒星形成。恒星形成率以及最近的恒星形成历史在中心区域同意与观测估计。这一新模型首次解释了最近第二次遭遇导致的北半球星系中核外恒星的形成。该模型预测，在合并阶段，黑猩猩比老鼠（NGC 4676）晚，因此将失去它们在经典Toomre序列中的第一位。
英文摘要：
We present a new high-resolution N-body/SPH simulation of an encounter of two gas-rich disk galaxies which closely matches the morphology and kinematics of the interacting Antennae galaxies (NGC 4038/39). The simulation includes radiative cooling, star formation and feedback from SNII. The large-scale morphology and kinematics are determined by the internal structure and the orbit of the progenitor disks. The properties of the central region, in particular the starburst in the overlap region, only match the observations for a very short time interval of ~20 Myr after the second encounter. This indicates that the Antennae galaxies are in a special phase only about 40 Myr after the second encounter and 50 Myr before their final collision. This is the only phase in the simulation when a gas-rich overlap region between the nuclei is forming accompanied by enhanced star formation. The star formation rate as well as the recent star formation history in the central region agree well with observational estimates. For the first time this new model explains the distributed extra-nuclear star formation in the Antennae galaxies as a consequence of the recent second encounter. The proposed model predicts that the Antennae are in a later merger stage than the Mice (NGC 4676) and would therefore lose their first place in the classical Toomre sequence.
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