Fig. 5.
Distribution of orbital eccentricities (see Eq. (1)) of migrating stars selected in the red box in Fig. 2. The eccentricities are calculated by using apocenters and pericenters of stellar orbits measured in different 1 Gyr time intervals, as mentioned in each frame. The mean value of eccentricity tends to decrease in time, and low-eccentricity stars start to appear after 3 Gyr.
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