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Formation of the Optical Spectra of L Dwarfs

  • Conference paper
Ultracool Dwarfs

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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Authors and Affiliations

  1. Main Astronomical Observatory of NAS, Golosiiv woods, 03680, Kyiv-127, Ukraine

    Y. Pavlenko

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  1. Y. Pavlenko
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Editors and Affiliations

  1. Astrophysics Research Institute, TwelveQuays House, Egerton Wharf, Birkenhead, CH41 1LD, UK

    Hugh R. A. Jones  & Iain A. Steele  & 

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© 2001 Springer-Verlag Berlin Heidelberg

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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

  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-642-62682-1

  • Online ISBN: 978-3-642-56672-1

  • eBook Packages: Springer Book Archive

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