T. R. White, T. R. Bedding, D. Stello, T. Appourchaux, J. Ballot, O. Benomar, A. Bonanno, A.-M. Broomhall, T. L. Campante, W. J. Chaplin, J. Christensen-Dalsgaard, E. Corsaro, G. Doǧan, Y. Elsworth, S. T. Fletcher, R. A. García, P. Gaulme, R. Handberg, S. Hekker, D. Huber, C. Karoff, H. Kjeldsen, S. Mathur, B. Mosser, M. J. P. F. G. Monteiro, C. Régulo, D. Salabert, V. Silva Aguirre, M. J. Thompson, G. A. Verner, R. L. Morris, D. T. Sanderfer, S. E. Seader
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 (ϵ). These measurements allow us to construct asteroseismic diagrams, namely the so-called C-D diagram of δν02 versus Δν, and the recently reintroduced ϵ 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 ϵ and Teff that allows for the unambiguous determination of radial order and should help resolve the problem of mode identification in F stars.
The Astrophysical Journal Letters
Volume 742, Number 1, Page L3_1