A major optical flare on the recently discovered X-ray active dMe star G 102-21.

Details A major optical flare on the recently discovered X-ray active dMe star G 102-21. A major optical flare on the recently discovered X-ray active dMe star G 102-21.

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...318..467p&link_type=abstract

Astronomy and Astrophysics, v.318, p.467-471

Astronomy and Astrophysics

Astrophysics

10

Stars: Activity, Stars: Flare, Stars: Individual: G 102-21, X-Rays: Stars

Scientific paper

During the course of UBV photoelectric measurements made at the Catania Astrophysical Observatory we have observed an unusually intense optical flare on the nearby M dwarf G 102-21, the optical counterpart of a strong X-ray source recently detected by ROSAT. The amplitude of the magnitude increase ({DELTA}U~7.3mag) and the total energy release in the UBV bands (E_UBV_~(1.4+/-0.3)x10^35^erg) put this event among the strongest flares ever detected on UV Ceti-type stars. The U-B and B-V colours of the flare emission did not significantly change during most of the flare development. While the B-V is quite a typical colour for stellar flares, the U-B is much bluer when compared with typical values given in literature. This unusually strong ultraviolet component of the flare emission, together with the very fast flare decay, suggest a possible flare site close to the limb. We find that the observed amount of flare energy could be explained by the fast release of energy stored in a magnetic filament located in between the two G 102-21 stellar components, with a surface magnetic field >=3600G. The characteristics of the quiescent optical emission are also discussed.

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