  We study environmental quenching in the Eagle}/C-Eagle cosmological
hydrodynamic simulations over the last 11 Gyr (i.e. $z=0-2$). The simulations
are compared with observations from the SAMI Galaxy Survey at $z=0$. We focus
on satellite galaxies in galaxy groups and clusters ($10^{12}\,\rm M_{\odot}$
$\lesssim$ $M_{200}$ < $3 \times 10^{15}\, \rm M_{\odot}$). A star-formation
concentration index [$C$-index $= \log_{10}(r_\mathrm{50,SFR} /
r_\mathrm{50,rband})$] is defined, which measures how concentrated star
formation is relative to the stellar distribution. Both Eagle/C-Eagle and SAMI
show a higher fraction of galaxies with low $C$-index in denser environments at
$z=0-0.5$. Low $C$-index galaxies are found below the SFR-$M_{\star}$ main
sequence (MS), and display a declining specific star formation rate (sSFR) with
increasing radii, consistent with ``outside-in'' environmental quenching.
Additionally, we show that $C$-index can be used as a proxy for how long
galaxies have been satellites. These trends become weaker at increasing
redshift and are absent by $z=1-2$. We define a quenching timescale $t_{\rm
quench}$ as how long it takes satellites to transition from the MS to the
quenched population. We find that simulated galaxies experiencing
``outside-in'' environmental quenching at low redshift ($z=0\sim0.5$) have a
long quenching timescale (median $t_{\rm quench}$ > 2 Gyr). The simulated
galaxies at higher redshift ($z=0.7\sim2$) experience faster quenching (median
$t_{\rm quench}$ < 2Gyr). At $z\gtrsim 1-2$ galaxies undergoing environmental
quenching have decreased sSFR across the entire galaxy with no ``outside-in''
quenching signatures and a narrow range of $C$-index, showing that on average
environmental quenching acts differently than at $z\lesssim 1$.
