  Galaxies arrive on the red sequences of clusters at high redshift ($z>1$)
once their star formation is quenched and evolve passively thereafter. However,
we have previously found that cluster red sequence galaxies (CRSGs) undergo
significant morphological evolution subsequent to the cessation of star
formation, at some point in the past 9-10~Gyr. Through a detailed study of a
large sample of cluster red sequence galaxies spanning $0.2<z<1.4$ we elucidate
the details of this evolution. Below $z \sim 0.5-0.6$ (in the last 5-6 Gyr)
there is little or no morphological evolution in the population as a whole,
unlike in the previous 4-5 Gyrs. Over this earlier time (i) disk-like systems
with S{\'e}rsic $n < 2$ progressively disappear, as (ii) the range of their
axial ratios similarly decreases, removing the most elongated systems (those
consistent with thin disks seen at an appreciable inclination angle), and (iii)
radial colour gradients (bluer outwards) decrease in an absolute sense from
significant age-related gradients to a residual level consistent with the
metallicity-induced gradients seen in low redshift cluster members. The
distribution of their effective radii shows some evidence of evolution,
consistent with growth of {\it at most} a factor $<1.5$ between $z\sim 1.4$ and
$z \sim 0.5$, significantly less than for comparable field galaxies, while the
distribution of their central ($<1$kpc) bulge surface densities shows no
evolution at least at $z<1$. A simple model involving the fading and thickening
of a disk component after comparatively recent quenching (after $z\sim 1.5$)
around an otherwise passively evolving older spheroid component is consistent
with all of these findings.
