  The basic processes of the formation of the first stars in the primordial
Universe are outlined and the implications for cosmological structure formation
discussed. By employing theoretical and numerical models of cosmic structure
evolution embedded within N-body hydrodynamical chemistry simulations,
predictions for the production of the first heavy elements in the Universe are
given. These results are then compared against measured data of UV luminosities
and metal abundances in different kinds of observations in order to draw
conclusions on the chemical and thermal state of the cosmic medium at different
cosmological epochs.
