  The primordial elements, H, He and Li are included in a low temperature
equation of state and monochromatic opacity function. The equation of state and
opacity function are incorporated into the stellar evolution code NG-ELMS,
which makes use of a non-grey model atmosphere computed at runtime. NG-ELMS is
used to compute stellar evolution models for primordial and lithium free
element mixtures, for stars in the sub-Solar mass range 0.8--0.15 Msol. We find
that lithium has little or no effect upon the structure and observable
properties of of stars in this mass range. Furthermore lithium is completely
destroyed by fusion before the main sequence in stars of mass less than ~0.7
Mol. We find that on the red giant branch and Hayashi track, the use of a
non-grey model atmosphere to provide the upper boundary conditions for the
stellar evolution calculation, results in significantly cooler less luminous
stars, across the mass range
