The Na I D resonance lines in main sequence late-type stars

Astronomy and Astrophysics – Astrophysics

Scientific paper

Rate now

  [ 0.00 ] – not rated yet Voters 0   Comments 0

Details

12 pages, including 14 figures and 4 tables. Accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2007.11833.x

We study the sodium D lines (D1: 5895.92 \AA; D2: 5889.95 \AA) 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 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.

No associations

LandOfFree

Say what you really think

Search LandOfFree.com for scientists and scientific papers. Rate them and share your experience with other people.

Rating

The Na I D resonance lines in main sequence late-type stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The Na I D resonance lines in main sequence late-type stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Na I D resonance lines in main sequence late-type stars will most certainly appreciate the feedback.

Rate now

     

Profile ID: LFWR-SCP-O-699420

  Search
All data on this website is collected from public sources. Our data reflects the most accurate information available at the time of publication.