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Model of Slowly Evolving Flare

Published online by Cambridge University Press:  27 September 2017

F. Chiuderi Drago ,
M. Landini  and
B.C. Monsignori Fossi
F. Chiuderi Drago
Affiliation:
Institute of Astronomy, University of Florence, Italy
M. Landini
Affiliation:
Department of Physics, University of Naples, Italy
B.C. Monsignori Fossi
Affiliation:
Arcetri Astrophysical Observatory, Florence, Italy

Abstract

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A gradual rise and fall flare, with a duration of about one hour was observed on June 10, 1980 in the radio (Toyokawa and VLA), optical (Bing Bear) and XUV (SMM satellite) ranges of wavelengths. The flare developed as a large loop connecting two regions of opposite polarity in a pre-exisisting active region. A model of the differential emission measure of the loop observed at three different stage of the flare is deduced from the analysis of the XUV images in C IV (1549 A), O VIII (18.97 A), Ne IX (13.45 A), Mg XI (9.17 A) and Si XIII (6.65 A) emission lines. The differential emission measure as a function of temperature is controlled by the conductive flux via the temperature gradient; the evaluation of the divergence of the conductive flux is used in the energy balance to have information on the power deposition function.

Type
Session II: Solar Flares
Information
International Astronomical Union Colloquium , Volume 104 , Issue 2: Solar and Stellar Flares , 1989 , pp. 195 - 198
Copyright
Copyright © Kluwer 1989

References

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Rosner, R., Tucker, W.H. and Vaiana, G.S., 1978, Ap.J., 220, 643 Google Scholar