Conveners
Tuesday - Session 3
- Iris Dillmann
How elements are made in the Universe is an open long-standing question. Several processes are invoked to explain the observed elemental abundances in our Solar System [1] and in our galaxy [2].
Complex astrophysical simulations are used to study the origin of the heavy elements and quantify the contribution of the r-process to the observed elemental abundances (see e.g. [3]). The r-process...
The lighter heavy elements of the first r-process peak, between strontium and silver, can be synthesized in the moderately neutron rich neutrino–driven ejecta of either core–collapse supernovae or neutron star mergers via the weak r–process [1]. This nucleosynthesis scenario exhibits uncertainties from the absence of experimental data from $(\alpha,xn)$ reactions on neutron–rich nuclei, which...
The r-process has been shown to be robust in reproducing the abundance distributions of heavy elements seen in ultra-metal poor stars. In contrast, observations of elements in the range 36 ≤ Z ≤ 47 display overabundances relative to r-process model predictions [1]. A proposed solution to this discrepancy is an additional source of early nucleosynthesis that preferentially produces the lighter...
