Volume 515, June 2010
|Number of page(s)||13|
|Section||Stellar structure and evolution|
|Published online||11 June 2010|
LESIA, UMR8109, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195 Meudon Cedex, France e-mail: email@example.com
2 Astronomy Unit, Queen Mary, University of London Mile End Road, London E1 4NS, UK
3 Instituto de Astrofísica de Canarias, 38205, La Laguna, Tenerife, Spain
4 Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
5 Indian Institute of Astrophysics, Koramangala, Bangalore 560034, India
6 Institut d'Astrophysique Spatiale, UMR8617, Université Paris XI, Bâtiment 121, 91405 Orsay Cedex, France
7 Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot; CEA, IRFU, SAp, centre de Saclay, 91191, Gif-sur-Yvette, France
8 GEPI, Observatoire de Paris, CNRS, Université Paris Diderot; 5 place Jules Janssen, 92190 Meudon, France
Accepted: 8 March 2010
Context. The star HD 49385 is the first G-type solar-like pulsator observed in the seismology field of the space telescope CoRoT. The satellite collected 137 days of high-precision photometric data on this star, confirming that it presents solar-like oscillations. HD 49385 was also observed in spectroscopy with the NARVAL spectrograph in January 2009.
Aims. Our goal is to characterize HD 49385 using both spectroscopic and seismic data.
Methods. The fundamental stellar parameters of HD 49385 are derived with the semi-automatic software VWA, and the projected rotational velocity is estimated by fitting synthetic profiles to isolated lines in the observed spectrum. A maximum likelihood estimation is used to determine the parameters of the observed p modes. We perform a global fit, in which modes are fitted simultaneously over nine radial orders, with degrees ranging from = 0 to = 3 (36 individual modes).
Results. Precise estimates of the atmospheric parameters (Teff, [M/H], log g) and of the ν sin i of HD 49385 are obtained. The seismic analysis of the star leads to a clear identification of the modes for degrees = 0,1,2. Around the maximum of the signal (ν 1013 μHz), some peaks are found significant and compatible with the expected characteristics of = 3 modes. Our fit yields robust estimates of the frequencies, linewidths and amplitudes of the modes. We find amplitudes of ~5.6 ± 0.8 ppm for radial modes at the maximum of the signal. The lifetimes of the modes range from one day (at high frequency) to a bit more than two days (at low frequency). Significant peaks are found outside the identified ridges and are fitted. They are attributed to mixed modes.
Key words: methods: data analysis / methods: statistical / methods: observational / stars: oscillations / stars: individual: HD 49385
Based on data obtained from the CoRoT (Convection, Rotation and planetary Transits) space mission, developed by the French Space agency CNES in collaboration with the Science Programs of ESA, Austria, Belgium, Brazil, Germany and Spain.
© ESO, 2010
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