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II/55 Gershberg Flare Star Catalogue (Shakhovskaya 1971)
The following files can be converted to FITS (extension .fit or fit.gz)
catalog.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=II/55
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Beginning of ReadMe :II/55 Gershberg Flare Star Catalogue (Shakhovskaya 1971)
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Gershberg Flare Star Catalogue
Shakhovskaya N.I.
<Veroeff. Bamberg IX, 138 (1971)>
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ADC_Keywords: Stars, flare
Description:
This catalog groups the flare stars as presented in the IAU Colloquium
15 (combined Colloquium of Commisions 27 and 42) held at Bamberg
31-Aug to 03-Sep 1971 entitled
"New Directions and New Frontiers in Variable Star Research"
The following definition of the UV Cet-type variables was given in
Kukarkin's General Catalogue of Variable Stars (1969): "dMe stars,
sometimes subject to flares with the amplitude from 1 to 6mag. Maximum
brightness is attained in seconds or dozens of seconds after the
commencement of the flare; the star returns to its normal brightness
after several minutes, or dozens of minutes. A typical representative
is UV Ceti." Now it is impossible to consider this definition as a
quite right because: 1) There are a number of M-dwarf stars affected
by the flares similar to the UV Ceti flares, but in their quiet state
spectra, no emission lines are observed. For example, BD+43 44A, BD+43
44 B, and SZ UMa, the flare activity of these stars were detected in
Crimea; and probably BD-04 4048B is suspected as a flare star by
HERBIG. 2) The lower limit of flare amplitude cited in Kukarkin's
corresponds to visual observations, but the modern photoelectric
observations register flares with amplitudes to 0.02-0.05mag.
Therefore we suppose, that UV Cet-type variables are K-M dwarfs, which
show quick flares with amplitudes exceeding the observational errors,
and duration of the flares are from a few seconds up to a few hundred
minutes.
The "catalog" file includes only such variable K-M dwarf stars, for
which existing observations allow to construct flare light curves. All
stars in "catalog", except V371 Ori, have photoelectric flare light
curves. The strong flare of V371 Ori was observed in radio region, but
simultaneous optical observations were carried out photographically
and visually only.