  Ram pressure stripping (RPS) is known to be a key environmental effect that
can remove interstellar gas from galaxies in a cluster. The RPS process is
commonly described as a competition between the ram pressure by the
intracluster medium (ICM) and the anchoring pressure on the interstellar medium
(ISM) by the gravitational potential of a galaxy. However, the actual gas
stripping process can be more complicated due to the complexity of gas physics
such as compression and geometrical self-shielding as well as cooling and
heating. In order to verify how well the observed signatures of the RPS process
can be understood as simple momentum transfer, we compare the stripping radii
of Virgo cluster galaxies in different stages of RPS measured from the HI
observation with the predicted gas truncation radii for the given conditions.
For the sample undergoing active RPS, we generally find good agreements between
predictions and observations within a measurement uncertainty. On the other
hand, galaxies likely in the early or later RPS stage and/or the ones with
signs of environmental impacts other than RPS such as tidal interaction or
starvation, show some discrepancies. Our results imply that the conventional
RPS relation works reasonably well in a broad sense when RPS is the most
dominant process and the galaxy is located where the surrounding environment
can be well defined. Otherwise, more careful inspections on the second
mechanism and local environment are required to assess the impact of RPS on the
target.
