  The equivalent widths of MgII absorption in the circumgalactic medium (CGM)
trace the global star formation rate up to $z<6$, are larger for star-forming
galaxies than passively-evolving galaxies, and decrease with increasing
distance from the galaxy. We delve further into the physics involved by
investigating gas kinematics and cloud column density distributions as a
function of galaxy color, redshift, and projected distance from the galaxy
(normalized by galaxy virial radius, $D/R_{\rm vir}$). For 39 isolated galaxies
at $0.3<z_{\rm gal}<1.0$, we have detected MgII absorption in high-resolution
($\Delta v\simeq 6.6$ km/s) spectra of background quasars within a projected
distance of $7<D<190$ kpc. We characterize the absorption velocity spread using
pixel-velocity two-point correlation functions. Velocity dispersions and cloud
column densities for blue galaxies do not differ with redshift nor with
$D/R_{\rm vir}$. This suggests that outflows continually replenish the CGM of
blue galaxies with high velocity dispersion, large column density gas out to
large distances. Conversely, absorption hosted by red galaxies evolves with
redshift where the velocity dispersions (column densities) are smaller (larger)
at $z_{\rm gal}<0.656$. After taking into account larger possible velocities in
more massive galaxies, we find that there is no difference in the velocity
dispersions or column densities for absorption hosted by red galaxies with
$D/R_{\rm vir}$. Thus, a lack of outflows in red galaxies causes the CGM to
become more quiescent over time, with lower velocity dispersions and larger
column densities towards lower $z_{\rm gal}$. The quenching of star formation
appears to affect the CGM out to $D/R_{\rm vir}=0.75$.
