Barban, C & Mosser, B

The Kepler space mission has observed many solar-like pulsators, and helped to decipher their main characteristics (e.g: mass, radius, rotation). Most of the achievements recently obtained in that domain consist of the analysis of the mode frequency positions. However, unique information on non-adiabatic physics derives from the height and width of the modes. In this study, we aim to measure the mode widths in thousands of Kepler red giants and to analyze their behavior in function of stellar parameters as well as seismic parameters. The results unveil a clear dependence on mass and stellar evolution for the star mode width, thus their mode damping.