  Taking advantage of the now available Gaia EDR3 parallaxes, we carry out an
archival {\it Hubble Space Telescope} (HST) far ultraviolet spectroscopic
analysis of 10 cataclysmic variable systems, including 5 carefully selected
eclipsing systems. We obtain accurate white dwarf (WD) masses and temperatures,
in excellent agreement with the masses for 4 of the eclipsing systems. For
three systems in our sample, BD Pav, HS 2214, and TT Crt, we report the first
robust masses for their WDs. We modeled the absorption lines to derive the WD
chemical abundances and rotational velocities for each of the ten systems. As
expected, for five higher inclination ($i \gtrsim 75^{\circ}$) systems, the
model fits are improved with the inclusion of a cold absorbing slab (an iron
curtain masking the WD) with $N_{\rm H} \approx 10^{20}-10^{22}$cm$^{-2}$.
Modeling of the metal lines in the HST spectra reveals that 7 of the 10 systems
have significant subsolar carbon abundance, and six have subsolar silicon
abundance, thereby providing further evidence that CV WDs exhibit subsolar
abundances of carbon and silicon. We suggest that strong aluminum absorption
lines (and iron absorption features) in the spectra of some CV WDs (such as IR
Com) may be due to the presence of a {\it thin} iron curtain ($N_{\rm H}\approx
10^{19}$cm$^{-2}$) rather than to suprasolar aluminum and iron abundances in
the WD photosphere. The derived WD (projected) rotational velocities all fall
in the range $\approx 100-400$~km/s, all sub-Keplerian similar to the values
obtained in earlier studies.
