  Using the EAGLE suite of simulations, we demonstrate that both cold gas
stripping {\it and} starvation of gas inflow play an important role in
quenching satellite galaxies across a range of stellar and halo masses,
$M_{\star}$ and $M_{200}$. By quantifying the balance between gas inflows,
outflows, and star formation rates, we show that even at $z=2$, only
$\approx30\%$ of satellite galaxies are able to maintain equilibrium or grow
their reservoir of cool gas - compared to $\approx50\%$ of central galaxies at
this redshift. We find that the number of orbits completed by a satellite is a
very good predictor of its quenching, even more so than the time since infall.
On average, we show that intermediate-mass satellites with $M_{\star}$ between
$10^{9}{\rm M}_{\odot}-10^{10}{\rm M}_{\odot}$ will be quenched at first
pericenter in massive group environments, $M_{200}>10^{13.5}{\rm M}_{\odot}$;
and will be quenched at second pericenter in less massive group environments,
$M_{200}<10^{13.5}{\rm M}_{\odot}$. On average, more massive satellites
($M_{\star}>10^{10}{\rm M}_{\odot}$) experience longer depletion time-scales,
being quenched between first and second pericenters in massive groups; while in
smaller group environments, just $\approx30\%$ will be quenched even after two
orbits. Our results suggest that while starvation alone may be enough to slowly
quench satellite galaxies, direct gas stripping, particularly at pericenters,
is required to produce the short quenching time-scales exhibited in the
simulation.
