Star Formation and Quenching of Satellite Galaxies
  We study the quenching of satellite galaxies by gradual depletion of gas due
to star formation, by ram-pressure striping and by tidally triggered starburst.
Using progenitors constrained by the empirical model of Lu et al., in which
outflow loading factor is low, we do not find an over-quenching problem in
satellites even if there is no further cold gas supply from the cooling of the
halo gas after a galaxy is accreted by its host. Gradual depletion alone
predicts a unimodal distribution in specific star formation, in contrast to the
bimodal distribution observed, and under-predicts the quenched fraction in low
mass halos. Ram-pressure stripping nicely reproduces the bimodal distribution
but under-predicts the quenched fraction in low-mass halos. Starbursts in
gas-rich satellites triggered by tidal interactions with central galaxies can
nicely reproduce the quenched satellite population in low-mass halos, but
become unimportant for low-mass satellites in massive halos. The combined
processes, together with the constrained progenitors, can reproduce the
observed star formation properties of satellites in halos of different masses.
