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We study the BELs in a sample of 11 gravitationally lensed quasars with atleast two epochs of observation to identify intrinsic variability and todisentangle it from microlensing. To improve our statistical significance wealso include 15 systems with single-epoch spectra. MgII and CIII] emissionlines are only weakly affected by microlensing, but CIV shows strongmicrolensing in some cases, even for regions of the line core, associated withsmall 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 inthe BLR, one that is insensitive to microlensing (of size $\gtrsim$ 50light-days and kinematics not confined to a plane) and another that shows uponly when it is magnified by microlensing (of size of a few light-days,comparable to the accretion disk). Both regions can contribute in differentproportions to the emission lines of different species and, within each lineprofile, to different velocity bins, all of which complicates detailed studiesof the BLR based on microlensing size estimates. The strength of themicrolensing indicates that some spectral features that make up thepseudo-continuum, such as the shelf-like feature at {\lambda}1610 or severalFeIII blends, may in part arise from an inner region of the accretion disk. Inthe case of FeII, microlensing is strong in some blends but not in others. Thisopens up interesting possibilities to study quasar accretion disk kinematics.

Microlensing and Intrinsic Variability of the Broad Emission Lines of Lensed Quasars