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Thimothy R. Bedding 1 Hans Kjeldsen 2 Tiago L. Campante 2, 3 Thierry Appourchaux 4 Alfio Bonanno 5 William J. Chaplin 6 Rafael A. Garcia 7 Milena Martic 8 Benoit Mosser 9, 10 R. Paul Butler 11 Hans Bruntt 1, 12 László L. Kiss 1, 13 Simon J. O'Toole 14 Eiji Kambe 15 Hiroyasu Ando 16 Hideyuki Izumiura 15 Bun'Ei Sato 17 Michael Hartmann 18 Artie Hatzes 18 Caroline Barban 12 Gabrielle Berthomieu 19 Eric Michel 12 Janine Provost 19 Sylvaine Turck-Chièze 7 Jean-Claude Lebrun 8 Jérôme Schmitt 20 Jean-Loup Bertaux 21 Serena Benatti 22 Riccardo U. Claudi 23 Rosario Cosentino 5 Silvio Leccia 24 Søren Frandsen 2 Karsten Brogaard 2 Lars Glowienka 2 Frank Grundahl 2 Eric Stempels 25 Torben Arentoft 2 Michaël Bazot 2 Jørgen Christensen-Dalsgaard 2 Thomas H. Dall 26 Christoffer Karoff 2 Jens Lundgreen-Nielsen 2 Fabien Carrier 27 Patrick Eggenberger 28 Danuta Sosnowska 28 Robert A. Wittenmyer 29, 30 Michael Endl 30 Travis S. Metcalfe 31 Saskia Hekker 6 Sabine Reffert 32
LATMOS - Laboratoire Atmosphères, Milieux, Observations Spatiales
Abstract : We have analyzed data from a multi-site campaign to observe oscillations in the F5 star Procyon. The data consist of high-precision velocities that we obtained over more than three weeks with 11 telescopes. A new method for adjusting the data weights allows us to suppress the sidelobes in the power spectrum. Stacking the power spectrum in a so-called échelle diagram reveals two clear ridges, which we identify with even and odd values of the angular degree (l = 0 and 2, and l = 1 and 3, respectively). We interpret a strong, narrow peak at 446 μHz that lies close to the l = 1 ridge as a mode with mixed character. We show that the frequencies of the ridge centroids and their separations are useful diagnostics for asteroseismology. In particular, variations in the large separation appear to indicate a glitch in the sound-speed profile at an acoustic depth of ~1000 s. We list frequencies for 55 modes extracted from the data spanning 20 radial orders, a range comparable to the best solar data, which will provide valuable constraints for theoretical models. A preliminary comparison with published models shows that the offset between observed and calculated frequencies for the radial modes is very different for Procyon than for the Sun and other cool stars. We find the mean lifetime of the modes in Procyon to be 1.29+0.55 -0.49 days, which is significantly shorter than the 2-4 days seen in the Sun.
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Thimothy R. Bedding, Hans Kjeldsen, Tiago L. Campante, Thierry Appourchaux, Alfio Bonanno, et al.. A MULTI-SITE CAMPAIGN TO MEASURE SOLAR-LIKE OSCILLATIONS IN PROCYON. II. MODE FREQUENCIES. The Astrophysical Journal, American Astronomical Society, 2010, 713 (2), pp.935-949. ⟨10.1088/0004-637X/713/2/935⟩. ⟨hal-00475239⟩



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