2006/12/16 by S. Leccia, H. Kjeldsen, A. Bonanno +4 · 18 citations
Earth and Planetary Sciences · Engineering · Physics and Astronomy · #Amplitude #Equivalent width #Geophysics and Sensor Technology #High-pressure geophysics and materials #Line (geometry) #Mode (computer interface) #Noise (video) #Pulsars and Gravitational Waves Research #Spectral density #Spectral line #Spectrograph #Telescope #astro-ph
paper · pdf · doi:10.1051/0004-6361:20066369
published in Astronomy and Astrophysics 464(3), 1059-1067 (EDP Sciences) · 10 pages, 15 figures, 4 tables. Accepted for publication in A&A
arxiv created 2006/12/16 · openalex publication_date 2007/01/11 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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.