Volume 547, November 2012
|Number of page(s)||8|
|Published online||06 November 2012|
Astronomical Observatory, Odessa National University, and Isaac Newton
Institute of Chile,
Odessa Branch, T.G. Shevchenko Park,
2 Université Bordeaux 1 – CNRS – Laboratoire d’Astrophysique de Bordeaux, UMR 5804, 33271 Floirac Cedex, France
3 Sternberg State Astronomical Institute, Lomonosov Moscow State University, 13, Universitetsky Av., 119991 Moscow, Russia
4 Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation of Russian Academy of Sciences (IZMIRAN), Troitsk, 142190 Moscow, Russia
Received: 7 November 2011
Accepted: 1 October 2012
Aims. The aim of the present study is to determine the Li abundances for a large set of the FGK dwarfs and to analyse the connections between the Li content, stellar parameters, and activity.
Methods. The atmospheric parameters, rotational velocities and the Li abundances were determined from a homogeneous collection of the echelle spectra with high resolution and a high signal-to-noise ratio. The rotational velocities vsini were determined by calibrating the cross-correlation function. The effective temperatures Teff were estimated by the line-depth ratio method. The surface gravities log g were computed by two methods: the iron ionization balance and the parallax. The LTE Li abundances were computed using synthetic spectra method. The behaviour of the Li abundance was examined in correlation with Teff, [Fe/H] , as well as with vsini and the level of activity in three stellar groups of the different temperature range.
Results. The stellar parameters and the Li abundances are presented for 150 slow rotating stars of the lower part of the main sequence. The studied stars show a decline in the Li abundance with decreasing temperature Teff and a significant spread, which should be due to the difference of age of stars. The correlations between the Li abundances, rotational velocities vsini, and the level of the chromospheric activity were discovered for the stars with 6000 > Teff > 5700 K, and it is tighter for the stars with 5700 > Teff > 5200 K. The target stars with Teff < 5200 K do not show any correlation between log A(Li) and vsini. The relationship between the chromospheric and coronal fluxes in active with detected Li as well as in less active stars gives a hint that there exist different conditions in the action of the dynamo mechanism in those stars.
Conclusions. We found that the Li-activity correlation is evident only in a restricted temperature range and the Li abundance spread seems to be present in a group of low chromospheric activity stars that also show a broad spread in the chromospheric vs. coronal activity.
Key words: stars: abundances / stars: activity / stars: late-type / stars: fundamental parameters / stars: rotation
Based on the spectra collected with the ELODIE spectrograph using the 1.93-m telescope at the Observatoire de Haute Provence (CNRS, France).
Full Table 3 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/547/A106
© ESO, 2012
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