The NaI D resonance lines in main-sequence late-type stars
Abstract
We study the sodium D lines (D1: 5895.92Å D2: 5889.95Å) in late-type dwarf stars. The stars have spectral types between F6 and M5.5 (B - V between 0.457 and 1.807) and metallicity between [Fe/H] = -0.82 and 0.6. We obtained medium-resolution echelle spectra using the 2.15-m telescope at the Argentinian observatory Complejo Astronómico El Leoncito (CASLEO). The observations have been performed periodically since 1999. The spectra were calibrated in wavelength and in flux. A definition of the pseudo-continuum level is found for all our observations. We also define a continuum level for calibration purposes. The equivalent width of the D lines is computed in detail for all our spectra and related to the colour index (B - V) of the stars. When possible, we perform a careful comparison with previous studies. Finally, we construct a spectral index (R'D) as the ratio between the flux in the D lines and the bolometric flux. We find that, once corrected for the photospheric contribution, this index can be used as a chromospheric activity indicator in stars with a high level of activity. Additionally, we find that combining some of our results, we obtain a method to calibrate in flux stars of unknown colour.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- July 2007
- DOI:
- 10.1111/j.1365-2966.2007.11833.x
- arXiv:
- arXiv:0704.0812
- Bibcode:
- 2007MNRAS.378.1007D
- Keywords:
-
- stars: activity;
- stars: chromospheres;
- stars: late-type;
- Astrophysics
- E-Print:
- 12 pages, including 14 figures and 4 tables. Accepted for publication in MNRAS