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Quasar outflows have been posited as a mechanism to couple super-massiveblack holes to evolution in their host galaxies. We use multi-epoch spectrafrom the Hubble Space Telescope and ground-based observatories to study theoutflows in seven quasars that have CIV outflow lines ranging from a classicBAL 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 andweakening plus the emergence of a new BAL system at $-$38,800 km/s accompaniedby dramatic strengthening in a mini-BAL at $-$22,800 km/s. We infer from$\sim$1:1 doublet ratios in PV and other lines that the BAL system is highlysaturated with line-of-sight covering fractions ranging from 0.27 to 0.80 inthe highest to lowest column density regions, respectively. Three of themini-BALs also provide evidence for saturation and partial covering based on$\sim$1:1 doublet ratios. We speculate that the BALs and mini-BALs form insimilar clumpy/filamentary outflows, with mini-BALs identifying smaller orfewer clumps along our lines of sight. If we attribute the line variabilitiesto clumps crossing our lines of sight at roughly Keplerian speeds, then atypical 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 andminimum 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 isin the range believed to be sufficient for feedback to galaxy evolution.

HST and Ground-Based Spectroscopy of Quasar Outflows: From Mini-BALs to BALs