Relatore
Benjamin Wehmeyer
(North Carolina State University)
Descrizione
The origin of the heaviest elements is still a matter of debate. For the rapid neutron capture process (r -process), multiple sites have been proposed, e.g., neutron star mergers and (sub-classes) of supernovae. R-process elements have been measured in a large fraction of metal-poor stars. Galactic archaeology studies show that the r-process abundances among these stars vary by over 2 orders of magnitude. On the other hand,abundances in stars with solar-like metallicity do not differ greatly. This leads to two major open questions: 1. What is the reason for such a huge abundance scatter of r -process elements in the early galaxy? 2. While the large scatter at low metallicities might point to a rare production site, why is there barely any scatter at solar metallicities? We use the high resolution ( 20 parsec/cell) inhomogeneous chemical evolution tool ”ICE” to study the role of the contributing source(s) of r-process elements. In this talk, I will discuss chemical evolution scenarios that provide an explanation for the observed abundance features of r-process elements in our Galaxy.
Autore principale
Benjamin Wehmeyer
(North Carolina State University)
Coautore
Carla Frohlich
(North Carolina State University)
F. K. Thielemann
(Universität Basel)
M. Pignatari
(University of Hull)
