Introduction and First Results
R. L. Gilliland, T. M. Brown, J. Christensen-Dalsgaard, H. Kjeldsen, C. Aerts, T. Appourchaux, S. Basu, T. R. Bedding, W. J. Chaplin, M. S. Cunha, P. De Cat, J. De Ridder, J. A. Guzik, G. Handler, S. D. Kawaler, L. L. Kiss, K. Kolenberg, D. W. Kurtz, T. S. Metcalfe, M. J. P. F. G. Monteiro, R. Szabů, T. Arentoft, L. A. Balona, J. Debosscher, Y. Elsworth, P.-O. Quirion, D. Stello, J.-C. SuŠrez, W. J. Borucki, J. M. Jenkins, D. Koch, Y. Kondo, D. W. Latham, J. F. Rowe, J. H. Steffen
Asteroseismology involves probing the interiors of stars and quantifying their global properties, such as radius and age, through observations of normal modes of oscillation. The technical requirements for conducting asteroseismology include ultra-high precision measured in photometry in parts per million, as well as nearly continuous time series over weeks to years, and cadences rapid enough to sample oscillations with periods as short as a few minutes. We report on results from the first 43 days of observations in which the unique capabilities of Kepler in providing a revolutionary advance in asteroseismology are already well in evidence. The Kepler asteroseismology program holds intrinsic importance in supporting the core planetary search program through greatly enhanced knowledge of host star properties, and extends well beyond this to rich applications in stellar astrophysics.
Publications of the Astronomical Society of the Pacific
Volume 122, Number 888, Page 131