Spectra of very low-luminosity red dwarfs

Details Spectra of very low-luminosity red dwarfs Spectra of very low-luminosity red dwarfs

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985aj.....90.2296p&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 90, Nov. 1985, p. 2296-2302.

Astronomy and Astrophysics

Astronomy

6

M Stars, Red Dwarf Stars, Spectrum Analysis, Stellar Luminosity, Stellar Spectra, Abundance, Balmer Series, Binary Stars, Flare Stars, Stellar Color, Stellar Magnitude, Ultraviolet Spectra, Visible Spectrum

Scientific paper

Spectra of seven M dwarfs are presented. Five stars have absolute visual magnitudes fainter than 14. UV Cet, V780 Tau, and G9-38 are active flare star binaries with hydrogen Balmer lines and the Ca II H and K lines prominently in emission. G158-27 and G171-10 have Mv about 15, but show no emission lines at the spectral resolution of 11 Å. This contradicts an earlier view that all late M dwarfs are active emission-line stars. Within the spectral range from 3500 to 6500 Å there are numerous TiO bandheads, as well as features due to MgH and CaH. The triatomic molecule CaOH is detected in the faintest stars of the sample. Most molecular bandheads correlate in strength with color index, suggesting that they are not completely saturated with respect to temperature sensitivity. The effects of emission lines on the B-V color index are large enough to separate dMe from dM stars.

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