Oscillating K Giants with the Wire Satellite: Determination of Their Asteroseismic Masses

Mass estimates of K giants are generally very uncertain. Traditionally, stellar masses of single field stars are determined by comparing their location in the Hertzsprung-Russell diagram with stellar evolutionary models. Applying an additional method to determine the mass is therefore of significant interest for understanding stellar evolution. We present the time series analysis of 11 K giants recently observed with the WIRE satellite. With this comprehensive sample, we report the first confirmation that the characteristic acoustic frequency, νmax, can be predicted for K giants by scaling from the solar acoustic cut-off frequency. We are further able to utilize our measurements of νmax to determine an asteroseismic mass for each star with a lower uncertainty compared to the traditional method, for most stars in our sample. This indicates good prospects for the application of our method on the vast amounts of data that will soon come from the COROT and Kepler space missions. Subject headings: stars: fundamental parameters — stars: oscillations — stars: interiors