1209.5696 (S. Mathur et al.)

Study of HD 169392A observed by CoRoT and HARPS    [PDF]

S. Mathur, H. Bruntt, C. Catala, O. Benomar, G. R. Davies, R. A. Garcia, D. Salabert, J. Ballot, B. Mosser, C. Regulo, W. J. Chaplin, Y. Elsworth, R. Handberg, S. Hekker, L. Mantegazza, E. Michel, E. Poretti, M. Rainer, I. W. Roxburgh, R. Samadi, M. Steslicki, K. Uytterhoeven, G. A. Verner, M. Auvergne, A. Baglin, S. Barcelo Forteza, F. Baudin, T. Roca Cortes

The numerous results obtained with asteroseismology thanks to space missions such as CoRoT and Kepler are providing a new insight on stellar evolution. After five years of observations, CoRoT is going on providing high-quality data. We present here the analysis of the double star HD169392 complemented by ground-based spectroscopic observations. This work aims at characterizing the fundamental parameters of the two stars, their chemical composition, the acoustic-mode global parameters including their individual frequencies, and their dynamics. We have analysed HARPS observations of the two stars to retrieve their chemical compositions. Several methods have been used and compared to measure the global properties of acoustic modes and their individual frequencies from the photometric data of CoRoT. The new spectroscopic observations and archival astrometric values suggest that HD169392 is a wide binary system weakly bounded. We have obtained the spectroscopic parameters for both components, suggesting the origin from the same cloud. However, only the mode signature of HD169392 A has been measured within the CoRoT data. The signal-to-noise ratio of the modes in HD169392B is too low to allow any confident detection. We were able to extract mode parameters of modes for l=0, 1, 2, and 3. The study of the splittings and inclination angle gives two possible solutions with splittings and inclination angles of 0.4-1.0 muHz and 20-40 degrees for one case and 0.2-0.5 muHz and 55-86 degrees for the other case. The modeling of this star with the Asteroseismic Modeling Portal led to a mass of 1.15+/-0.01 Ms, a radius of 1.88+/-0.02 Rs, and an age of 4.33+/-0.12 Gyr, where the uncertainties are the internal ones.

View original: http://arxiv.org/abs/1209.5696