Three-body recombination in primordial star formation

Three-body recombination and its importance to first star formation will be discussed. Published rates for molecular hydrogen formation disagree by several orders of magnitude at temperatures relevant to primordial gas. This uncertainty limits the reliability of gravitational collapse models at high densities. An overview of various approaches for calculating three-body recombination rates and the status of current efforts to improve these rates for H and He will be presented.