  Quasar outflows have been posited as a mechanism to couple super-massive
black holes to evolution in their host galaxies. We use multi-epoch spectra
from the Hubble Space Telescope and ground-based observatories to study the
outflows in seven quasars that have CIV outflow lines ranging from a classic
BAL to weaker/narrower "mini-BALs" across rest wavelengths of at least 850
$\AA$ to 1650 $\AA$. The CIV outflow lines all varied within a time frame of
$\leq$ 1.9 yrs (rest). This includes equal occurrences of strengthening and
weakening plus the emergence of a new BAL system at $-$38,800 km/s accompanied
by dramatic strengthening in a mini-BAL at $-$22,800 km/s. We infer from
$\sim$1:1 doublet ratios in PV and other lines that the BAL system is highly
saturated with line-of-sight covering fractions ranging from 0.27 to 0.80 in
the highest to lowest column density regions, respectively. Three of the
mini-BALs also provide evidence for saturation and partial covering based on
$\sim$1:1 doublet ratios. We speculate that the BALs and mini-BALs form in
similar clumpy/filamentary outflows, with mini-BALs identifying smaller or
fewer clumps along our lines of sight. If we attribute the line variabilities
to clumps crossing our lines of sight at roughly Keplerian speeds, then a
typical variability time in our study, $\sim$1.1 yrs, corresponds to a distance
$\sim$2 pc from the central black hole. Combining this with the speed and
minimum total column density inferred from the PV BAL, $N_H \gtrsim$
2.5$\times$10$^{22}$ cm$^{-2}$, suggests that the BAL outflow kinetic energy is
in the range believed to be sufficient for feedback to galaxy evolution.
