C abundances in G and K nearby stars (Da Silva+, 2011)

Details C abundances in G and K nearby stars (Da Silva+, 2011) C abundances in G and K nearby stars (Da Silva+, 2011)

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010ycat..35269071d&link_type=abstract

VizieR On-line Data Catalog: J/A+A/526/A71. Originally published in: 2011A&A...526A..71D

Physics

Atomic Physics

Stars: Nearby, Stars: Atmospheres, Abundances, Atomic Physics

Scientific paper

The files atmmol.dat and atmstrg.dat contain tables with a and molecular line parameters required by the MOOG code (Kurucz, 1995ASPC...81..CD18) to compute synthetic spectra: the rest wavelength, the line identification, the excitation potential of lower level, the oscillator strength, and the dissociation energy (only for molecular features). The line parameters of the following spectral regions are listed: from 5115 to 5170 Angstroms, containing the C2 molecular band head around 5128 and 5165; from 5360 to 5390 Angstroms, containing the Carbon atomic line at 5380.3; and the region from 5195 to 5225 Angstroms, which was also used to treat the C2 molecular band head around 5165.
The opacity contributions of strong atomic lines can be distinctly considered by the MOOG code. Therefore, strong lines are listed in a separate file (atm_strg.dat).
The data was taken from Kurucz (1995ASPC...81..CD18) and from the Vienna Atomic Line Database (VALD - Kupka et al. 2000BaltA...9..590K, Kupka et al. 1999A&AS..138..119K, Piskunov et al. 1995A&AS..112..525P, Ryabchikova et al. 1997BaltA...6..244R), using the "Extract Stellar" option for Teff=5777K, logg=4.44, microturbulence=1.0km/s, and a detection limit of 0.001 (which means that lines with central depths <0.1% of the continuum were rejected). In order to fit the solar spectrum, a correction factor of 0.85 was applied for C2 lines, and a correction factor of 0.5 for MgH lines. The oscillator strength values of some atomic and molecular lines were also revised when needed.
The file cfe_3reg.dat contains individual Cabon abundance ratios with respect to Iron, together with their errors, computed from the three C abundance indicators studied here: the C2 molecular band head around 5128 and 5165 Angstroms, and the C atomic line at 5380.3 Angstroms.
(3 data files).

Affiliated with

Also associated with

No associations

Rating

C abundances in G and K nearby stars (Da Silva+, 2011) 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 C abundances in G and K nearby stars (Da Silva+, 2011), we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and C abundances in G and K nearby stars (Da Silva+, 2011) will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1533924