The Effect of the Electron Donor H+3 on the Pre-Main-Sequence and Main-Sequence Evolution of Low-Mass, Zero-Metallicity Stars

H has been shown (1991 work of Lenzuni and coworkers) to be the dominant positive ion in a zero-metallicity gas at low temperature and intermediate to high density. It therefore affects both the number of free electrons and the opacity of the gas. The most recent H partition function (1995 work of Neale & Tennyson) is an order of magnitude larger at 4000 K than all previous partition functions, implying that H is a more important electron donor than previously thought. Here we present new Rosseland mean opacities for a hydrogen-helium gas of 1000 K ≤ T ≤ 9000 K and -14 ≤[ρ (g cm-3)] ≤ -2. In the calculation of these opacities, we have made use of the latest collision-induced absorption data as well as the most recent H partition function and line opacity data. It is shown that these updated and new sources of opacity give rise to a Rosseland mean opacity for a hydrogen-helium gas that is, in general, greater than that calculated in earlier works. The new opacity data are then used to model the evolution of low-mass (0.15-0.8 M☉), zero-metallicity stars, from pre-main-sequence collapse to main-sequence turnoff. To investigate the effect of H on the evolution of low-mass, zero-metallicity stars, we repeat our calculations neglecting H as a source of electrons and line opacity. We find that H can have an effect on the structure and evolution of stars of mass ~0.5 M☉ or less. A gray atmosphere is used for the calculation, which is sufficient to demonstrate that H affects the evolution of very low mass stars to a greater degree than previously believed.