Oscillations in Procyon A: First results from a multi-site campaign
| Titre | Oscillations in Procyon A: First results from a multi-site campaign |
| Type de publication | Journal Article |
| Year of Publication | 2008 |
| Auteurs | Hekker, S, Arentoft, T, Kjeldsen, H, Bedding, TR, Christensen-Dalsgaard, J, Reffert, S, Bruntt, H, Butler, RP, Kiss, LL, O'Toole, SJ, Kambe, E, Ando, H, Izumiura, H, Sato, B, Hartmann, M, Hatzes, AP, Appourchaux, T, Barban, C, Berthomieu, G, Bouchy, F, Garcia, RA, Lebrun, J-C, Martic, M, Michel, E, Mosser, B, Nghiem, PAP, Provost, J, Samadi, R, Thévenin, F, Turck-Chieze, S, Bonanno, SA, Benatti, S, Claudi, RU, Cosentino, R, Leccia, S, Frandsen, S, Brogaard, K, Grundahl, F, Stempels, HC, Bazot, M, Dall, TH, Karoff, C, Carrier, F, Eggenberger, P, Sosnowska, D, Wittenmyer, RA, Endl, M, Metcalfe, TS |
| Journal | Journal of Physics Conference SeriesJournal of Physics Conference Series |
| Volume | 118 |
| Pagination | 2059 |
| Date Published | October 1, 2008 |
| Résumé | Procyon A is a bright F5IV star in a binary system. Although the distance, mass and angular diameter of this star are all known with high precision, the exact evolutionary state is still unclear. Evolutionary tracks with different ages and different mass fractions of hydrogen in the core pass, within the errors, through the observed position of Procyon A in the Hertzsprung-Russell diagram. For more than15 years several different groups have studied the solar-like oscillations in Procyon A to determine its evolutionary state. Although several studies independently detected power excess in the periodogram, there is no agreement on the actual oscillation frequencies yet. This is probably due to either insufficient high-quality data (i.e., aliasing) or due to intrinsic properties of the star (i.e., short mode lifetimes). Now a spectroscopic multi-site campaign using 10 telescopes world-wide (minimizing aliasing effects) with a total time span of nearly 4 weeks (increase the frequency resolution) is performed to identify frequencies in this star and finally determine its properties and evolutionary state. |
