  We discuss two aspects of the ionization and abundances in QSO intrinsic
absorbers. First, we use the high-ionization doublet Ne VIII 770,780 to test
the relationship between the UV line absorbers and the ``warm'' absorbers
detected in soft X-rays. In one well-measured QSO with intrinsic z_a ~ z_e
lines, UM 675, we estimate that the UV absorber has at least 10 times too
little O VII and O VIII to produce the requisite bound-free edges at ~0.8 keV.
Second, we show that firm lower limits on the metal-to-hydrogen abundances can
be established even with no constraints on the ionization. Those lower limits
are typically Z ~> Z_o and sometimes Z ~> 10 Z_o (e.g. for the BALs). We argue
that QSO metallicities up to at least ~9 Z_o are consistent with the rapid
early-epoch star formation expected in the cores of massive galaxies.
