  We present a time variability analysis of broad absorption lines (BAL; spread
over the velocity range of 5800-29000 km/s) seen in the spectrum of
J132216.25+052446.3 (z(em)= 2.04806) at ten different epochs spanning over 19
years. The strongest absorption component (BAL-A; spread over 5800-9900 km/s)
is made up of several narrow components having velocity separations close to C
IV doublet splitting. The C IV, N V, and Si IV absorption from BAL-A show
correlated optical depth variability without significant changes in the
velocity structure. A very broad and shallow absorption (BAL-C; spread over the
velocity range 15000-29000 km/s) emerged during our monitoring period
coinciding with a dimming episode of J1322+0524. All the identified absorption
lines show correlated variability with the equivalent widths increasing with
decreasing flux. This together with the C IV emission-line variability is
consistent with ionization being the main driver of the correlated variability.
The observed UV-continuum variations are weaker than what is required by the
photo-ionization models. This together with a scatter in the C iv equivalent
width at a given continuum flux can be understood if variations of the C IV
ionizing photons are much larger than that of the UV continuum, the variations
in the ionizing photon and UV fluxes are not correlated and/or the covering
factor of the flow varies continuously. We suggest BAL-A is produced by a
stable clumpy outflow located beyond the broad emission line region and BAL-C
is a newly formed wind component located near the accretion disk and both
respond to changes in the ionizing continuum.
