Hydrodynamic simulations of an isolated star-forming gas cloud in the
  Virgo cluster
  We present a suite of three-dimensional, high-resolution hydrodynamic
simulations that follow the evolution of a massive (10^7 M_sun) pressure
confined, star-forming neutral gas cloud moving through a hot intra-cluster
medium (ICM). The main goal of the analysis is to get theoretical insight into
the lifetimes and evolution of stellar systems like the recently discovered
star-forming cloud SECCO~1 in the Virgo cluster of galaxies, but it may be of
general interest for the study of the star-forming gas clumps that are observed
in the tails of ram pressure stripped galaxies. Building upon a previous,
simple simulation, we explored the effect of different relative velocity of the
cloud and larger temperature of the ICM, as well as the effect of the cloud
self-gravity. Moreover, we performed a simulation including star-formation and
stellar feedback, allowing for a first time a direct comparison with the
observed properties of the stars in the system. The survivability of the cold
gas in the simulated clouds is granted on timescales of the order of 1 Gyr,
with final cold gas fractions generally $>0.75$. In all cases, the simulated
systems end up, after 1 Gyr of evolution, as symmetric clouds in pressure
equilibrium with the external hot gas. We also confirm that gravity played a
negligible role at the largest scales on the evolution of the clouds. In our
simulation with star formation, star formation begins immediately, it peaks at
the earliest times and decreases monotonically with time. Inhomogeneous
supernova explosions are the cause of an asymmetric shape of the gas cloud,
facilitating the development of instabilities and the decrease of the cold gas
fraction.
