类似Milky Way的椎间盘运动学中小合并的特征：振铃的再研究
Signatures of minor mergers in Milky Way-like disc kinematics: Ringing revisited
摘要：
通过N体模拟，我们研究了星系盘对较小合并事件的响应。我们发现，非自引力，螺旋状的功能诱导厚盘。正如我们在以前的工作中所展示的，这种“振铃”也会在小的空间区域（如太阳附近）的速度空间（u-v平面）中留下印记。当圆盘在事件发生后松弛时，u-v平面上的团块随着时间的推移而越来越近，这使我们能够估计撞击的时间。除了确认这种诊断的可能性，在这里，我们表明，在一个更现实的情况下，在下降轨迹的扰动引起的方位角依赖的结构在相空间。我们还发现，由恒星的能量和角动量定义的空间是比速度空间更好的选择，因为即使在大的局部体积中，团块仍然可见。这使得它们的观测检测更加容易，因为人们不需要被限制在一个小的空间体积。我们表明，信息的影响时间，质量的扰动，其轨迹存储在盘星的运动学。
英文摘要：
By means of N-body simulations we study the response of a galactic disc to a minor merger event. We find that non-self-gravitating, spiral-like features are induced in the thick disc. As we have shown in a previous work, this "ringing" also leaves an imprint in velocity space (the u-v plane) in small spatial regions, such as the solar neighbourhood. As the disc relaxes after the event, clumps in the u-v plane get closer with time, allowing us to estimate the time of impact. In addition to confirming the possibility of this diagnostic, here we show that in a more realistic scenario, the in-fall trajectory of the perturber gives rise to an azimuthal dependence of the structure in phase-space. We also find that the space defined by the energy and angular momentum of stars is a better choice than velocity space, as clumps remain visible even in large local volumes. This makes their observational detection much easier since one need not be restricted to a small spatial volume. We show that information about the time of impact, the mass of the perturber, and its trajectory is stored in the kinematics of disc stars.
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