Institution(s): 1. Facultad de Ciencias, UNAM, 2. Instituto de Astronomia-UNAM
The preliminary results of an asteroseismic analysis of the red giant star KIC 5701829 observed for 29 d in short-cadence mode with the Kepler satellite are reported. The oscillation spectrum of this star is characterized by the presence of a well-defined solar-like oscillation pattern due to radial acoustic modes. The high-precision time series data allow us to accurately extract the oscillation frequencies from the power spectrum. The characterization of the power spectrum has been performed following three basics steps commonly used in the analysis of solar-like oscillations: fitting and correcting for the background, estimating the frequency of maximum power (nu_max) and the large separation (Dnu), and extracting individual frequencies. We find that the frequency of maximum oscillation power ,nu_max, and the mean large frequency separation, Dnu, are around 143 and 12 muHz, respectively.
In order to shed more light on the structure of KIC 5701829 a seismic modeling have been carried out. The physical parameters of the stars have been derived from Stromgren photometry and spectroscopic observations. We have computed a grid of theoretical structure models for the star and the adiabatic oscillation frequencies for all the models satisfying the observational constraints. As a result we find that the star is still ascending the red-giant branch.