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arped disk galaxies are classified into two morphologies: S- and U-types.Conventional theories routinely attribute both types to galactic tidalinteraction and/or gas accretion, but reproducing of U-types in simulations isextremely challenging. Here we investigate whether both types are governed bythe same mechanisms using the most extensive sample of $\sim$8000 nearby(0.02\,$<$\,z\,$<$\,0.06) massive ($M_{*}/M_{\odot}$\,$>$\,$10^9$) edge-ondisks from SDSS. We find that U-types show on average bluer optical colors andhigher specific star formation rate (sSFR) than S-types, with more stronglywarped U-types having higher sSFR. We also find that while the S-type warpproperties correlate with the tidal force by the nearest neighbor regardless ofthe environment, there is no such correlation for U-types in groups/clusters,suggesting a non-tidal environmental could be at play for U-types, such as rampressure stripping (RPS). Indeed, U-types are more common in groups/clustersthan in fields and they have stellar mass, gas fraction, sSFR enhancement andphase-space distribution closely analogous to RPS-induced jellyfish galaxies inclusters. We furthermore show that the stellar disks of most RPS galaxies inthe IllustirsTNG simulation are warped in U-shape and bent in oppositedirection of stripped gas tails, satisfying theoretical expectations forstellar warps embeded in jellyfishes. We therefore suggest that despite themajority of U-types that live in fields being still less explained, RPS can bean alternative origin for those in groups/clusters.

Warped Disk Galaxies. I. Linking U type Warps in Groups/Clusters to Jellyfish Galaxies