  We study the BELs in a sample of 11 gravitationally lensed quasars with at
least two epochs of observation to identify intrinsic variability and to
disentangle it from microlensing. To improve our statistical significance we
also include 15 systems with single-epoch spectra. MgII and CIII] emission
lines are only weakly affected by microlensing, but CIV shows strong
microlensing in some cases, even for regions of the line core, associated with
small projected velocities. However, excluding the strongly microlensed cases,
there is a strikingly good match between the red wings of the CIV and CIII]
profiles. Analysis of these results supports the existence of two regions in
the BLR, one that is insensitive to microlensing (of size $\gtrsim$ 50
light-days and kinematics not confined to a plane) and another that shows up
only when it is magnified by microlensing (of size of a few light-days,
comparable to the accretion disk). Both regions can contribute in different
proportions to the emission lines of different species and, within each line
profile, to different velocity bins, all of which complicates detailed studies
of the BLR based on microlensing size estimates. The strength of the
microlensing indicates that some spectral features that make up the
pseudo-continuum, such as the shelf-like feature at {\lambda}1610 or several
FeIII blends, may in part arise from an inner region of the accretion disk. In
the case of FeII, microlensing is strong in some blends but not in others. This
opens up interesting possibilities to study quasar accretion disk kinematics.
