Abstract
Formation processes of spectra of low-mass stars and substellar objects (L dwarfs) with 1200 < Teff < 2200 K are discussed. We show that the overall shapes of their optical spectra are governed by the strong resonance lines of K I and Na I. Mechanisms of their broadening in stellar atmospheres of late spectral classes are analyzed. The computed spectral energy distributions (SED’s) of L dwarfs are compared to the observed spectra. Perspectives of Lithium and Deuterium tests to assess the new populations of the Galaxy have been considered.
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Pavlenko, Y. (2001). Formation of the Optical Spectra of L Dwarfs. In: Jones, H.R.A., Steele, I.A. (eds) Ultracool Dwarfs. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-56672-1_4
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DOI: https://doi.org/10.1007/978-3-642-56672-1_4
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