Solar-like Oscillations in KIC 11395018 and KIC 11234888 from 8 Months of Kepler Data
| Title | Solar-like Oscillations in KIC 11395018 and KIC 11234888 from 8 Months of Kepler Data |
| Publication Type | Journal Article |
| Year of Publication | 2011 |
| Authors | Mathur, S, Handberg, R, Campante, TL, Garcia, RA, Appourchaux, T, Bedding, TR, Mosser, B, Chaplin, WJ, Ballot, J, Benomar, O, Bonanno, A, Corsaro, E, Gaulme, P, Hekker, S, Regulo, C, Salabert, D, Verner, G, White, TR, Brandao, IM, Creevey, OL, Dogan, G, Elsworth, Y, Huber, D, Hale, SJ, Houdek, G, Karoff, C, Metcalfe, TS, Molenda-Zakowicz, J, Monteiro, MJPFG, Thompson, MJ, Christensen-Dalsgaard, J, Gilliland, RL, Kawaler, SD, Kjeldsen, H, Quintana, EV, Sanderfer, DT, Seader, SE |
| Journal | The Astrophysical Journal |
| Volume | 733 |
| Pagination | 95 |
| Date Published | June 1, 2011 |
| Keywords | asteroseismology, methods: data analysis, stars: individual: KIC 11395018 KIC 11234888, stars: oscillations, stars: solar-type |
| Abstract | We analyze the photometric short-cadence data obtained with the Kepler mission during the first 8 months of observations of two solar-type stars of spectral types G and F: KIC 11395018 and KIC 11234888, respectively, the latter having a lower signal-to-noise ratio (S/N) compared with the former. We estimate global parameters of the acoustic (p) modes such as the average large and small frequency separations, the frequency of the maximum of the p-mode envelope, and the average line width of the acoustic modes. We were able to identify and to measure 22 p-mode frequencies for the first star and 16 for the second one even though the S/N of these stars are rather low. We also derive some information about the stellar rotation periods from the analyses of the low-frequency parts of the power spectral densities. A model-independent estimation of the mean density, mass, and radius is obtained using the scaling laws. We emphasize the importance of continued observations for the stars with low S/N for an improved characterization of the oscillation modes. Our results offer a preview of what will be possible for many stars with the long data sets obtained during the remainder of the mission. |
