EDP Sciences
Free access
Volume 430, Number 2, February I 2005
Page(s) 669 - 677
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20041745

A&A 430, 669-677 (2005)
DOI: 10.1051/0004-6361:20041745

The Ca II Infrared Triplet as a stellar activity diagnostic

I. Non-LTE photospheric profiles and definition of the R $\mathsf{_{IRT}}$ indicator
V. Andretta1, I. Busà2, M. T. Gomez1 and L. Terranegra1

1  INAF - Osservatorio Astronomico di Capodimonte, salita Moiariello 16, 80131 Napoli, Italy
    e-mail: andretta@na.astro.it
2  INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95125 Catania, Italy

(Received 28 July 2004 / Accepted 21 September 2004 )

This work is part of a larger project on the study of activity in stars of spectral type similar to, or later than the Sun, from PMS to ZAMS, based on the analysis of the high resolution $\ion{Ca}{ii}$ InfraRed Triplet ( $\ion{Ca}{ii}$ IRT: $\lambda= 8498$, 8542, 8662 Å) observed profiles. Here, a preliminary study on the diagnostic power of these calcium lines has been performed by means of NLTE calculations of the line profiles with an approximate treatment of UV line-blanketing, for a grid of photospheric models with Teff = 4200, 5200, 6200 K, ${\log g}$ = 4.0, 4.5, 5.0 and [A/H] = 0.0, -1.0, -2.0. We used these calculations to estimate the sensitivity of the profiles to changes in stellar parameters and the effect of departures from LTE. As found by other authors, the $\ion{Ca}{ii}$ triplet NLTE EQWs (equivalent widths) are quite sensitive to photospheric parameters, in particular to Teff and [A/H]. On the other hand, we find that the dependence of the $\ion{Ca}{ii}$ triplet lines central depression (CD = 1-central relative flux) on ${\log g}$ and  Teff, and to a lesser extent to [A/H], is very weak. The departure from LTE is negligible when we consider EQWs, unless very metal-poor atmospheres are considered, while CDs can be affected by NLTE by more than 20%. This analysis indicates that in the use of these lines as activity indicators (where the details of the line profile in the core are important), a NLTE treatment is required. Furthermore, we show that a new chromospheric indicator, which we denote RIRT, can be derived from measurements of $\ion{Ca}{ii}$ IRT line central depressions, provided that rotational broadening is taken into proper account. In order to facilitate the use of the $\ion{Ca}{ii}$ IRT lines as activity diagnostics, we give interpolation formulae for estimating line CDs within the range of stellar parameters of our NLTE calculations.

Key words: stars: atmospheres -- stars: activity -- radiative transfer -- line: formation -- line: profiles -- stars: late-type

SIMBAD Objects

© ESO 2005