Theoretical Nuclear Astrophysics activities range from nuclear physics issues (e.g. cross section predictions for strong and weak interaction processes and properties of nuclei far from stability) to numerical simulations of explosive astrophysical events (e.g. supernovae , X-ray bursts, and binary neutron star mergers). A major focus exists on nucleosynthesis contributions of these objects to galactic evolution.
Macroscopic phenomena in nature - in astrophysics and on Earth - often originate from the interaction of tightly coupled microscopic processes with different characteristic length and time scales. We develop efficient transport/hydrodynamics algorithms in the context of gravitational collapse and supernova explosions. A reliable numerical link between the input physics and the observables in distant astrophysical objects provides new information about matter under otherwise inaccessible conditions, or vice versa, allows the prediction of a large-scale evolution based on well-known input physics.
Our group is representing traditional observational astronomy. Topics of interest range from wide binary star statistics in our Galaxy, the structure and distribution of dwarf galaxies, the morphology of galaxies in general, and near-field cosmology. Most of our recent work is based on the Sloan Digital Sky Survey database.
Our group interest is the understanding and the modelling of the synthesis of molecules and dust in our local and far universe from a theoretical point of view. We focus on the major dust providers in galaxies, i.e., stars in their late stages of evolution and develop chemical/physical models describing the formation of molecules and dust in evolved stellar environments. The resulting theoretical predictions are further tested by observations in the optical, infrared, submillimetre and millimetre ranges using telescope facilities worldwide.