Poster abstract details

With the advent of the Kepler mission, we are able to perform large-scale ensemble asteroseismology of main-sequence and subgiant stars for the first time. The relationship between asteroseismic observables, such as frequency spacings, can significantly constrain stellar parameters. We have computed evolutionary tracks for asteroseismic HR diagrams from models of varying mass and metallicity. For the first time we have extended the CD diagram beyond the main-sequence to the tip of the red giant branch. We also consider other possible asteroseismic diagrams that are more sensitive at different evolutionary stages. We compare the model evolutionary tracks in these diagrams with results from pre-Kepler studies of solar-like oscillations, and early results from the Kepler mission.