The formation of the first second generation star.

While the exact masses of the first stars are still unknown, it remains relatively well accepted that the Pop III initial mass function is not identical to that of stars forming today. This transition in star forming modes is due to the introduction of metals produced in the first supernovae. These metals enhance the radiative cooling efficiency of gas through fine-structure lines, molecular transitions, and thermal emission from dust grains. Simulations have made great contributions to our understanding of the ability of metals to induce fragmentation in collapsing gas, but little attention has been paid the actual conditions present when the Universe becomes enriched with metals for the first time. We present the results from a simulation of the formation of the first metal-enriched stars under realistic conditions. We simulate a Population III star forming halo and assume the formation of a 40 M⊙ metal-free star. Using 3D radiation hydrodynamics, we then compute the evolution of the HII region and the blast-wave of the subsequent core-collapse supernova. We then follow the simulation until the first metal-enriched prestellar clouds collapse. We report on the status of this ongoing simulation. [ABSTRACT FROM AUTHOR]