Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..608p&link_type=abstract
Astronomicheskij Zhurnal, vol. 74, p. 608
Astronomy and Astrophysics
Astronomy
1
M Stars, Lithium, Late Stars, Stellar Atmospheres, Brown Dwarf Stars, Stellar Spectra, Resonance Lines, Approximation, Atmospheric Models
Scientific paper
The results of numerical modeling of lithium lines in the spectra of late-type M dwarfs are discussed. Line-by-line and just-overlapping approximations are used to compute the molecular opacities. Synthetic spectra are computed near two lithium lines, a resonance line at 6708 A and a subordinate line at 8126 A, for a number of late-type M dwarfs using the model atmosphere grids of Allard and Hauschildt. The two molecular absorption models used yield very similar profiles for strong lithium lines that could in principle be observed in the spectra of brown dwarfs. Pseudoequivalent widths of lithium absorption lines are computed and compared with the equivalent widths in the spectrum of the brown dwarf candidate Teide1 measured by Rebolo et al. (1992). This comparison indicates that the lithium abundance in Teide1's atmosphere is high: lg N (Li) greater than 3.0 and lg N (Li) = 2.9 for 6708 and 8126 A, respectively. This provides strong evidence for identification of Teide1 as a brown dwarf.
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