The Evolution of Accreting Population III Stars at 10^-6-10³ M_/yr

The first stars formed over five orders of magnitude in mass by accretion in primordial dark matter halos. We study the evolution of massive, very massive and supermassive primordial (Pop III) stars over nine orders of magnitude in accretion rate. We use the stellar evolution code GENEC to evolve accreting Pop III stars from 10^-6 - 10³ M_/yr and study how these rates determine final masses. The stars are evolved until either the end of central Si burning or until they encounter the general relativistic instability (GRI). We also examine how metallicity affects the evolution of the stars. At rates below 2. 5 x 10^-5 M_/yr the final mass of the star falls below that required for pair-instability supernovae. The minimum rate required to produce black holes with masses above 250 M_ is 5 x 10^-5 M_/yr, well within the range of infall rates found in numerical simulations of halos that cool via H₂, 10^-3 M_/yr. At rates of 5 x 10^-5 M_/yr to 4 x 10^-2 \ yr^-1, like those expected for halos cooling by both H₂ and Ly-alpha, the star collapses after Si burning. At higher accretion rates the GRI triggers the collapse of the star during central H burning. Stars that grow at above these rates are cool red hypergiants with effective temperatures log (T₄₅₅) = 3. 8 and luminosities that can reach 10^10. 5 L_. At accretion rates of 100 - 1000 M_/yr the gas encounters the general relativistic instability prior to the onset of central hydrogen burning and collapses to a black hole with a mass of 10⁶ M_ without ever having become a star. We reveal for the first time the critical transition rate in accretion above which catastrophic baryon collapse, like that which can occur during galaxy collisions in the high-redshift Universe, produces supermassive black holes via dark collapse.