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We characterize the morphological properties of a statistically relevantsample of H$\alpha$ and UV young star-forming clumps and optical complexes,observed with the \textit{Hubble Space Telescope} in six galaxies of the GASPsample undergoing ram-pressure stripping. The catalogs comprise 2406 (323 inthe tails) H$\alpha$ clumps, 3750 (899) UV clumps and 424 tail opticalcomplexes. About 15-20\% of the clumps and 50\% of the complexes are resolvedin size. We find that more than half of the complexes contain no H$\alpha$clumps, while most of them contain at least one UV clump. The clump number andsize increase with the complex size, while the median complex filling factor islarger for UV clumps ($0.27$) than for H$\alpha$ clumps ($0.10$) and does notcorrelate with almost any morphological property. This suggests that the clumpsnumber and size grow with the complex keeping the filling factor constant. Whenstudying the position of the clumps inside their complexes, H$\alpha$ clumps,and UV clumps to a lesser extent, show a displacement from the complex centerof $0.1-1$ kpc and, in $\sim 60$\% of the cases, they are displaced away fromthe galactic disk. This is in accordance with the fireball configuration,already observed in the tails of stripped galaxies. Finally, the filling factorand the clump radius increase with the distance from the galactic disk,suggesting that the reciprocal displacement of the different stellargenerations increases as a consequence of the velocity gradient caused by rampressure.

Morphology of star-forming clumps in ram-pressure stripped galaxies as seen by HST