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Comparison of UV Ceti Flares with Solar Flares

Published online by Cambridge University Press:  14 August 2015

W. Haupt  and
W. Schlosser
W. Haupt
Affiliation:
Seminar für Technologie, Gesamthochschule Essen
W. Schlosser
Affiliation:
Astronomisches Institut, Ruhr Universität Bochum

Abstract

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During several intervals totalling 26 h, 84 flares of UV Ceti were observed using a photometer with 1 s time resolution. Using solar flare terminology, all flares of UV Ceti observed here can be characterized by a typical light curve, consisting of a preflare, a flash and a slow phase. Observations of Bopp and Moffett (1973) show that the flash phase of UV Ceti is dominated by continuous and Hα emission. UV Ceti flare flash phases are compared with solar ‘white-light’ emission during the flash phase and it is suggested that during all UV Ceti flares strong-particle emission occurs, as is the case for solar white-light flares (Švestka, 1970). The characteristics of the solar flare particles are similar to those of the soft cosmic ray sources (Mogro-Campero and Simpson, 1972). If all flare stars emit particles with these characteristics they could produce the soft cosmic ray component in agreement with the work of Comstock (1969).

Type
Part 1 / Flare Stars and T Tauri Stars
Information
Symposium - International Astronomical Union , Volume 67: Variable Stars and Stellar Evolution , 1975 , pp. 99 - 100
Copyright
Copyright © Reidel 1975 

References

References

Bopp, B. W. and Moffett, T. J.: 1973, Astrophys. J. 185, 239.CrossRefGoogle Scholar
Comstock, G. U.: 1969, Astrophys. J. 155, 619.Google Scholar
Mogro-Campero, A. and Simpson, J. A.: 1972, Astrophys. J. 177, L37.CrossRefGoogle Scholar
Švestka, Z.: 1970, Solar Phys. 13, 471.Google Scholar

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