Poster abstract details

Recent radial velocity surveys have discovered more than 30 extrasolar
planets orbiting giant stars. These discoveries are important because
the host stars have masses that are larger than the Sun. However, the
determination of the stellar mass of giant stars is difficult because
the evolutionary tracks of main sequence stars covering a wide range of
masses all converge to a small region of the HR diagram. Here we present
new results from the analysis of observed stellar oscillations of planet
hosting giant stars. The investigation of stellar oscillations for these
objects offers us the possibility to derive an independent determination
of the stellar mass which is important for extrasolar planet studies.