Speaker
Katharina Wollenberg
(Universität Heidelberg)
Description
J031300 is now the most metal-poor star discovered to date, with a maximum Fe abundance of 10^(-7.1) solar. Two possible Pop III supernova candidates have been identified, with progenitor masses of 12.4 and 60 Msun, whose nucleosynthetic yields that are a good match to the chemical abundances found in J031300. However, explaining the actual metallicity of J031300 also requires an understanding of how the metals produced by the first supernovae are diluted in the early IGM and later taken up into second-generation stars. We study this process, by modeling mixing in a primordial supernova remnant and its fragmentation into new stars using high-resolution numerical simulations. We employ the Kepler stellar evolution code to obtain models of the two low energy Pop III supernovae which match the chemical abundances of J031300, and we combine these results with 2D simulations of mixing and fragmentation in the supernova remnants at later times using the ZEUS-MP magnetohydrodynamics code.
Author
Katharina Wollenberg
(Universität Heidelberg)