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We investigate the formation of jellyfish galaxies usingradiation-hydrodynamic simulations of gas-rich dwarf galaxies with amulti-phase interstellar medium (ISM). We find that the ram-pressure-stripped(RPS) ISM is the dominant source of molecular clumps in the near wake within 10kpc from the galactic plane, while in-situ formation is the major channel fordense gas in the distant tail of the gas-rich galaxy. Only 20% of the molecularclumps in the near wake originate from the intracluster medium (ICM); however,the fraction reaches 50% in the clumps located at $80\,{\rm kpc}$ from thegalactic center since the cooling time of the RPS gas tends to be short due tothe ISM--ICM mixing ($\lesssim$ 10 Myr). The tail region exhibits a starformation rate of $0.001-0.01\,{\rm M_{\odot}\,yr^{-1}}$, and most of the tailstars are born in the stripped wake within 10 kpc from the galactic plane.These stars induce bright H$\alpha$ blobs in the tail, while H$\alpha$ tailsfainter than $6\times10^{38}\,{\rm erg\,s^{-1}\,kpc^{-2}}$ are mostly formedvia collisional radiation and heating due to mixing. We also find that thestripped tails have intermediate X-ray to H$\alpha$ surface brightness ratios(1.5$\lesssim F_{\rm X}/F_{\rm H\alpha}\lesssim$20), compared to the ISM($\lesssim$1.5) or pure ICM ($\gg$20). Our results suggest that jellyfishfeatures emerge when the ISM from gas-rich galaxies is stripped by strong rampressure, mixes with the ICM, and enhances the cooling in the tail.

Simulating Jellyfish Galaxies: A Case Study for a Gas-Rich Dwarf Galaxy