  Galactic destruction of primordial deuterium is inevitably linked through
star formation to the chemical evolution of the Galaxy. The relatively high
present gas content and low metallicity suggest only modest D-destruction. In
concert with deuterium abundances derived from solar system and/or interstellar
observations this suggests a primordial deuterium abundance in possible
conflict with data from some high-redshift, low-metallicity QSO absorbers. We
have explored a variety of chemical evolution models including infall of
processed material and early, supernovae-driven winds with the aim of
identifying models with large D-destruction which are consistent with the
observations of stellar-produced heavy elements. When such models are
confronted with data we reconfirm that only modest destruction of deuterium
(less than a factor of 3) is permitted. When combined with solar system and
interstellar data these results favor the low deuterium abundances derived for
the QSO absorbers observed by Tytler et al (1996) and by Burles & Tytler
(1996).
