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Stellar flare diagnostics from multi–wavelength observations

Published online by Cambridge University Press:  26 February 2010

Alexander V. Stepanov ,
Yuri T. Tsap  and
Yulia G. Kopylova
Alexander V. Stepanov
Affiliation:
Pulkovo Observatory, 196140 S.–Petersburg, Pulkovskoye chaussee 65/1, Russia email: stepanov@gao.spb.ru; yulia00@mail.ru
Yuri T. Tsap
Affiliation:
Pulkovo Observatory, 196140 S.–Petersburg, Pulkovskoye chaussee 65/1, Russia email: stepanov@gao.spb.ru; yulia00@mail.ru Crimean Astrophysical Observatory, 98409 Nauchny, Crimea, Ukraine email: yur@crao.crimea.ua
Yulia G. Kopylova
Affiliation:
Pulkovo Observatory, 196140 S.–Petersburg, Pulkovskoye chaussee 65/1, Russia email: stepanov@gao.spb.ru; yulia00@mail.ru
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Abstract

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Quasi–periodic pulsations in various wavebands are natural manifestations of emission of stellar flares. We suggest a diagnostic tool of stellar flares based on the coronal seismology and the solar–stellar analogy. Two approaches are used: (I) flare loop as a resonator for MHD oscillations and (II) flare loop as an equivalent electric circuit. Using optical, X–ray, and radio data we obtained flare plasma parameters for the red dwarfs EQ Peg, AT Mic, and AD Leo. The characteristic length of stellar flare loops l ~ R* and their electric currents turned out to be one–two orders of magnitude lager than the solar ones. Advantages of proposed diagnostics in comparison to the scaling law methods are given.

Keywords

stars: late–typeflareplasmasmagnetohydrodynamicsoscillationscoronae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S264: Solar and Stellar Variability: Impact on Earth and Planets , August 2009 , pp. 288 - 291
Copyright
Copyright © International Astronomical Union 2010

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