  We present stellar evolution models for 0.5 - 1.2 \Msol at scaled
metallicities of 0.1 - 1.5 Z\sol and O/Fe values of 0.44 - 2.28 O/Fe\sol. The
time dependent evolution of habitable zone boundaries are calculated for each
stellar evolution track based on stellar mass, effective temperature, and
luminosity parameterizations. The rate of change of stellar surface quantities
and the surrounding habitable zone position are strong functions of all three
quantities explored. The range of orbits that remain continuously habitable, or
habitable for at least 2 Gyr, are provided. The results show that the detailed
chemical characterization of exoplanet host stars and a consideration of their
evolutionary history are necessary to assess the likelihood that a planet found
in the instantaneous habitable zone has had sufficient time to develop a
biosphere capable of producing detectable biosignatures. This model grid is
designed for use by the astrobiology and exoplanet communities to efficiently
characterize the time evolution of host stars and their habitable zones for
planetary candidates of interest.
