Volume 464, Number 3, March IV 2007
|Page(s)||1059 - 1067|
|Section||Stellar structure and evolution|
|Published online||11 January 2007|
Seismology of Procyon A: determination of mode frequencies, amplitudes, lifetimes, and granulation noise
INAF – Astronomical Observatory of Capodimonte, Salita Moiariello 16, 80131 Napoli, Italy e-mail: email@example.com
2 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade, Building 1520, 8000 Aarhus C, Denmark
3 INAF – Astrophysical Observatory of Catania, via S. Sofia 78, 95123 Catania, Italy
4 INAF – Astronomical Observatory of Padua, Vicolo Osservatorio 5, 35122 Padova, Italy
5 Department of Physics and Astronomy, Astrophysics Section, University of Catania, via S. Sofia 78, 95123 Catania, Italy
Accepted: 7 December 2006
The F5 IV-V star Procyon A () was observed in January 2001 by means of the high-resolution spectrograph SARG operating with the TNG Italian telescope (Telescopio Nazionale Galileo) in the Canary Islands, exploiting the iodine cell technique. The time series of about 950 spectra carried out during 6 observation nights and a preliminary data analysis [CITE] showed a significant power excess between 0.5 and , with peak amplitude. Here we present a more detailed analysis of the time series, based on both radial velocity and line equivalent width analyses. From the power spectrum we found a typical p-mode frequency comb-like structure, identified 11 frequencies with a good margin of certainty in the interval of modes with and , and determined large and small frequency separations, and , respectively. The mean amplitude per mode () at peak power is , twice larger than the solar one, and the mode lifetime is , which indicates a non-coherent, stochastic source of mode excitation. Line equivalent width measurements do not show a significant excess in power in the examined spectral region but allowed us to infer an upper limit to the granulation noise.
Key words: stars: oscillations / stars: individual: Procyon A / techniques: spectroscopic / techniques: radial velocities
© ESO, 2007
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