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Fig. 4


First row: contour density plots of the final versus initial radii for all particles in different time spans for the gSb or gSa models, as indicated. The orange dashed line shows the locus of non-migrating, cold particles. Nonuniform deviations from this line indicate that there exist preferential radii where migration efficiency is stronger, however, these are not clearly seen. Second row: non-migrating stars, extracted from the distributions above as described in the text. Third row: the migrators only, obtained by subtracting the distributions in the second from those in the first row. The dotted-red and solid-blue vertical/horizontal lines in all panels indicate the positions of the bar’s CR and OLR, respectively, at the initial/final times. Strong clumps can now be seen across the bar’s CR for example. Fourth row: number density plots of the changes in angular momentum, ΔL, versus the initial angular momentum (or equivalently initial radius), L, divided by the rotational velocity at each radius. The broken red and blue vertical strips indicate the location of the bar’s CR and OLR, where their widths corresponding to the change during each time period. The pink lines connect some corresponding groups of migrated stars. The bar’s CR is active throughout the entire simulations.

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