  The galaxy quenching process, in which a galaxy stops forming stars is a
crucial stage in galaxy life. Two mechanisms for quenching are possible: halo
mass quenching of central galaxies and environmental quenching of satellite
galaxies. This thesis describes the satellite galaxies (SG) quenching process
and its primary causes. The analysis contains a study of a large sample of 118
SGs within the Vela cosmological simulation, identified by a specific SG merger
tree algorithm.
  We find that the quenching evolves through a typical path in the diagram of
specific star formation (sSFR) vs. inner stellar surface density
($\Sigma_{\star, 0.5\textrm kpc}$), with the inner surface density defined as
the density within 0.5kpc from the center of mass of the SG. Three discrete
phases characterize this path: 1. Halt in gas accretion with SG compaction at
high sSFR as the SG keeps forming stars 2. Gas removal and rapid drop in the
sSFR at the peri-center of its orbit within the host halo 3. Stellar heating
and stripping may lead to coalescing with the halo center, an ultra-diffuse
galaxy (UDG), a compact elliptical galaxy (eCg), or a globular cluster (GC).
  We find that the main drivers of SG evolution are ram pressure stripping at
the initial stages and tidal forces at the final stages, aided by starvation,
suppression of gas accretion. We show that other processes, such as gas
depletion by star formation or stellar feedback are secondary.
  Moreover, we present an innovative method for constructing merger trees in
simulations that solve systemic errors. Two new significant results presented
here: a. Decoupling of dark-matter from the stellar component in SGs. b.
Compact elliptical SG formation.
  An assembly of these results and others are presented in a fast and robust
catalog.
