Class: FlareStar

Flare Star

•owl:Thing
        •AstrObject
                •VariableObject
                        •EruptiveVariableStar
                                •FlareStar

Super Classes

EruptiveVariableStar

Annotations

misc:descriptionEruptive variables varying in brightness because of flares occurring in their chromospheres and coronae. Sub-types: - Orion variables of late (K-M) spectral types - Eruptive variables of the UV Ceti type, these are K Ve-M Ve stars sometimes displaying flare activity with amplitudes from several tenths of a magnitude up to 6 mag in V. The amplitude is considerably greater in the ultraviolet spectral region. Maximum light is attained in several seconds or dozens of seconds after the beginning of a flare; the star returns to its normal brightness in several minutes or dozens of minutes. - Flaring Orion variables of spectral types Ke-Me. These are phenomenologically almost identical to UV Cet variables observed in the solar neighborhood. In addition to being related to nebulae, they are normally characterized by being of earlier spectral type and greater luminosity, with slower development of flares (V389 Ori). - BY Draconis-type (rotating) variables, which are emission-line dwarfs of dKe-dMe spectral type showing quasiperiodic light changes with periods from a fraction of a day to 120 days and amplitudes from several hundredths to 0.5 mag in V. The light variability is caused by axial rotation of a star with a variable degree of nonuniformity of the surface brightness (spots) and chromospheric activity. Some of these stars also show flares similar to those of UV Cet stars, and in those cases they also belong to the latter type and are simultaneously considered eruptive variables.
simbad:nameFlare*
simbad:shortCodeFl*
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