  X-ray studies of jellyfish galaxies opened a window in the physics of the
interplay between intracluster medium (ICM) and interstellar medium (ISM). In
this paper, we present the study of an archival \textit{Chandra} observation of
the GASP jellyfish galaxy JO194. We observe X-ray emission extending from the
stellar disk to the unwinding spiral arms with an average temperature of
$kT=0.79\pm0.03$ keV. To investigate the origin of the X-ray emission, we
compare the observed X-ray luminosities with those expected from the star
formation rates (SFR) obtained from H$\alpha$ emission. We estimate an X-ray
luminosity excess of a factor $\sim2-4$ with respect to the SF, therefore we
conclude that SF is not the main responsible for the extended X-ray emission of
JO194. The metallicity in the spiral arms ($Z=0.24^{+0.19}_{-0.12} Z_{\odot}$)
is consistent with that of the ICM around JO194 ($Z=0.35\pm0.07$), thus we
suggest that the ICM radiative cooling dominates the X-ray emission of the
arms. We speculate that the X-ray plasma results from the ISM-ICM interplay,
although the nature of this interplay is still mostly unknown. Finally, we
observe that the X-ray properties of JO194 are consistent with those of two
other GASP galaxies with different stellar mass, phase-space conditions in
their hosting clusters, and local ICM conditions. We suggest that the
conditions required to induce extended X-ray emission in jellyfish galaxies are
established at the beginning of the stripping, and they can persist on long
time scales so that galaxies in different clusters and evolutionary stages can
present similar extended X-ray emission.
