Evolution of primordial H2 for different cosmological models

Primordial chemistry began in the recombination epoch when the adiabatic expansion caused the temperature of the radiation to fall below 4000 K. The chemistry of the early Universe involves the elements hydrogen, its isotope deuterium, helium with its isotopic forms and lithium. In this communication I will present results on the evolution of the primordial $H_2$ abundance for different cosmological models and the influence on the thermal decoupling.