Emisión Hα en sistemas binarios cromosféricamente activos (RS CVn y BY Dra)

Details Emisión Hα en sistemas binarios cromosféricamente activos (RS CVn y BY Dra) Emisión Hα en sistemas binarios cromosféricamente activos (RS CVn y BY Dra)

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992anfis..88...39f&link_type=abstract

Anales de Física, v.88, p.39-54 (1992)

Physics

2

Stars: Activity, Stars: Binaries, Stars: Chromospheres, Stars: Late-Type

Scientific paper

We report here high and medium resolution Balmer Hα line profiles for 11 chromospherically active binary systems including the class of RS Canum Venaticorum binaries (RS CVn) and BY Draconis (BY Dra) with a total range of rotation periods from 0.8 to 24 days. We have obtained different types of Hα line profiles: strong emission line, weak emission line with strong superposed absorption profile and filled-in absorption line profile. We have measured the Hα equivalent width of the program stars and the Hα core emission was determined by subtraction of the equivalent width of a presumably inactive star with the same spectral type and luminosity class.

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