  Radiation feedback from massive population III stars may have given rise to
low mass star formation from primordial or nearly primordial material. If early
universe low mass stars did form, some should remain locally as white dwarfs,
sub-giants, or main sequence stars. In this paper, we present model
calculations for the evolution of single 0.8 Msun to 3.0 Msun stars with
primordial metallicity from pre-main sequence to the white dwarf cooling track,
and calculations for the evolution of single 4.0 Msun to 7.0 Msun stars which
conclude in the giant phase. One goal of this work is to identify potential
observable markers for potential observed progenitors of first or nearly first
stars. We uncover a number of seemingly peculiar evolutionary differences
between that of pop III low mass stars compared with younger higher Z stars, as
well as compared to other primordial evolution models. We also present an
initial-final mass relationship and identify the minimum mass of a single white
dwarf that could have had a population III progenitor.
