Formation of the optical spectra of the coolest M- and L-dwarfs and lithium abundances in their atmospheres
| dc.creator | Pavlenko, Ya. V. | |
| dc.date | 2000-02-07 | |
| dc.date.accessioned | 2026-07-25T11:00:04Z | |
| dc.description | Theoretical aspects of modeling of spectra of late M- and L-dwarfs are discussed. We show, that the processes of formation of spectra of M- and L-dwarfs are basically different. Instead of the case of M-dwarfs, atoms of Ti and V should be depleted into grains in the atmospheres of L-dwarfs. Overall shape of the L-dwarf spectra is governed by the K I + Na I resonance line wings of the huge strength. To fit lithium lines observed in spectra of the coolest dwarfs we used two additional suggestions: a) there are some EXTRA depletions of molecular species absorbed in the optical spectra of L-dwarfs; b) there may be (a few?) additional (``dusty''?) opacity sources in their atmospheres. Problems of lithium line formation and the ``natural'' limitation of their use for the ``lithium test'' for the case of L-dwarfs are considered. | |
| dc.description | 6 pages, latex, 4 EPS figs, summary of talk at IAU Symposium 198: The Light Elements and their Evolution (Natal), ASP Conf. Series, 2000, eds. L. da Silva, M. Spite, and J.R. de Medeiros | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0002144 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0002144 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/487 | |
| dc.subject | Astrophysics | |
| dc.title | Formation of the optical spectra of the coolest M- and L-dwarfs and lithium abundances in their atmospheres | |
| dc.type | text |