Asteroseismic Diagrams from a Survey of Solar-like Oscillations with Kepler
|Title||Asteroseismic Diagrams from a Survey of Solar-like Oscillations with Kepler|
|Publication Type||Journal Article|
|Year of Publication||2011|
|Authors||White, TR, Bedding, TR, Stello, D, Appourchaux, T, Ballot, J, Benomar, O, Bonanno, A, Broomhall, A-M, Campante, TL, Chaplin, WJ, Christensen-Dalsgaard, J, Corsaro, E, Doğan, G, Elsworth, YP, Fletcher, ST, García, RA, Gaulme, P, Handberg, R, Hekker, S, Huber, D, Karoff, C, Kjeldsen, H, Mathur, S, Mosser, B, Monteiro, MJPFG, Régulo, C, Salabert, D, Aguirre, VSilva, Thompson, MJ, Verner, G, Morris, RL, Sanderfer, DT, Seader, SE|
|Journal||The Astrophysical Journal Letters|
|Date Published||November 1, 2011|
Photometric observations made by the NASA Kepler Mission have led to a dramatic increase in the number of main-sequence and subgiant stars with detected solar-like oscillations. We present an ensemble asteroseismic analysis of 76 solar-type stars. Using frequencies determined from the Kepler time-series photometry, we have measured three asteroseismic parameters that characterize the oscillations: the large frequency separation (Δν), the small frequency separation between modes of l = 0 and l = 2 (δν02), and the dimensionless offset (epsilon). These measurements allow us to construct asteroseismic diagrams, namely the so-called Christensen-Dalsgaard diagram of δν02 versus Δν, and the recently re-introduced epsilon diagram. We compare the Kepler results with previously observed solar-type stars and with theoretical models. The positions of stars in these diagrams places constraints on their masses and ages. Additionally, we confirm the observational relationship between epsilon and T eff that allows for the unambiguous determination of radial order and should help resolve the problem of mode identification in F stars.