A - 1180 Wien / Vienna
Österreich / Austria
Looking at our Sun's future
Stars like our Sun are producing energy by the fusion of
Hydrogen in their interior. However, the Hydrogen is not lasting
forever. In a few billion years our Sun will turn into a Red
Giant star with severe impacts on planet Earth. Then it will
start the final stages of its evolution. One of
these stages is called the AGB phase. We are studying
stars that are already in this phase. In this way we are taking
a look into the future of our Sun.
Observationally, we use photometry (individual observations or long-term
monitoring) as well as spectoscopy (low- to highest-resolution) in different
wavelengths (from the optical to IR and Radio) to study AGB stars (single stars
and members of whole populations like globular clusters or extragalactic
systems) and their properties.
On the theoretical side, we use radiation hydrodynamics to model the complexe
atmospheres of AGB stars and radiative transfer codes to calculate synthetic
spectra from the optical range to the IR.
For the identification of dust features in IR spectra of AGB stars, we use
spectroscopic data that we derive from laboratory investigations of minerals
and synthetic solids.
Schematic view of an AGB star - simple version
(by J. Hron)