The dynamical evolution of the stellar clumps in the Sparkler galaxy

Open Access

Fig. 9.

Fraction of the clump mass enclosed within the tidal radius defined as in Eq. (14). The masses of the clumps are 10⁶, 10⁷, and 10⁸ M_⊙ (dashed, dotted and solid lines, respectively). The effective radius of the clumps is given by Eq. (1). Tidal radii are computed for distances between 1 and 10 kpc.

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