Speaker
Description
We have recently investigated the origin of chemical signatures
observed in the oldest star of our Galaxy using a
stochastic chemical evolution model. The elements we have studied are
carbon, nitrogen, and oxygen, but also the neutron capture elements. We
have found that rotating massive stars are a promising way to explain
several signatures observed in these fossil stars. Analyzing the
chemical abundance characteristics of the extremely and ultra-metal-poor stars we also found that our model can be improved if we consider
the presence of faint supernovae. These results seem to imply that
rotating massive stars and faint supernovae scenarios complement each other, and are both required to match
the observed chemistry of the earliest phases of the chemical
enrichment of the Universe.
