  We use ZENS data at low redshift to study the dependence of the quenched
satellite fraction and of the morphological mix of these quenched satellites,
on three different environmental parameters: group halo mass, halo-centric
distance and large-scale structure over-density. The fraction of quenched
satellites is independent of halo mass and the surrounding large-scale
overdensity, but increases towards the centres of the haloes, as previously
found. The morphological mix is, however, constant with radial position,
indicating that the well-known morphology-density relation results from the
increasing fraction of quenched galaxies towards the centres of haloes. The
constancy of the morphological outcome suggests that mass-quenching and
satellite quenching have the same effect on the morphologies of the galaxies.
The quenched satellites have larger B/T and smaller half-light radii than the
star-forming satellites. These are mostly due to differences in the disks. The
bulges in quenched satellites have very similar luminosities and surface
brightness profiles, and any mass growth of the bulges associated with
quenching cannot greatly change these quantities. The quenched disks are
fainter and have smaller scale lengths than in star-forming satellites. This
can be explained either by a differential fading of the disks or if disks were
generally smaller in the past, both of which are expected in an inside-out
growth of disks. At least at low redshifts, the structure of massive quenched
satellites is produced by processes that operate before quenching takes place.
A comparison with semi-analytic models argues for a reduction in the efficiency
of group halos in quenching their disk satellites and for mechanisms to
increase the B/T of low mass quenched satellites. [abridged]
