  Ram-pressure stripping is a crucial evolutionary driver for cluster galaxies
and jellyfish galaxies, characterized by very extended tails of stripped gas,
are the most striking examples of it in action. Recently, those extended tails
are found to show on-going star formation raising the question how the
stripped, cold gas can survive long enough to form new stars outside the
stellar disk. In this work, we summarize the most recent results achieved
within the GASP collaboration to provide a holistic explanation for this
phenomenon. We focus on two textbook examples of jellyfish galaxies, JO206 and
JW100 for which, via multi-wavelength observations from radio to X-ray and
numerical simulations, we have explored the different gas phases (neutral,
molecular, diffuse-ionized, and hot). Based on additional multi-phase gas
studies we now propose a scenario of stripped tail evolution including all
phases that is driven by a magnetic draping sheath, where the intracluster
turbulent magnetized plasma condenses onto the galaxy disk and tail and
produces a magnetized interface that protects the stripped galaxy tail gas from
evaporation. In such a scenario, the accreted environmental plasma can cool
down and eventually join the tail gas, hence providing additional gas to form
stars. The implications of our findings can shed light on the more general
scenario of draping, condensation, and cooling of hot gas surrounding cold
clouds that is fundamental in many astrophysical phenomena.
