Chromospheric lines in red dwarf flare stars. II - EV Lacertae EQ Pegasi A, and V1054 Ophiuchi

Details Chromospheric lines in red dwarf flare stars. II - EV Lacertae EQ Pegasi A, and V1054 Ophiuchi Chromospheric lines in red dwarf flare stars. II - EV Lacertae EQ Pegasi A, and V1054 Ophiuchi

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..214p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 1, 1984, p. 214-225.

Astronomy and Astrophysics

Astrophysics

33

Binary Stars, Chromosphere, Flare Stars, H Alpha Line, Red Dwarf Stars, Stellar Spectrophotometry, Emission Spectra, Optical Thickness, Spectral Energy Distribution, Spectral Line Width, Spectral Resolution, Stellar Luminosity

Scientific paper

It is pointed out that the solar neighborhood red dwarf flare stars have bolometric luminosities between 1/10 and 1/1000 that of the sun. Pettersen and Coleman (1981) have studied chromospheric lines in the active flare star AD Leo and in the low-frequency, non-emission-line flare star GX And, both of which have luminosities about 1/40 that of the sun. The present investigation is concerned with observations of somewhat fainter stars, having luminosities 1/60-1/70 that of the sun. The considered stars belong to the set of red dwarfs which have masses in the range from 0.3 to 0.4 solar mass and develop a radiative core at ages in the range from 10 to the 7th to 10 to the 8th yr. Attention is given to the star parameters, details regarding the stars, instrumentation and observational procedures, the H-alpha emission line, the Na I D lines, the He I lines, the Li I lines, and the Ca II infrared triplet lines.

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