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Modelling a Solar Flare from X-UV and Radio Observations

Published online by Cambridge University Press:  19 July 2016

F. Chiuderi Drago  and
B.C. Monsignori Fossi
F. Chiuderi Drago
Affiliation:
Department of Astronomy and Space Science, University of Florence Largo Enrico Fermi 5 - 50125 Florence, Italy
B.C. Monsignori Fossi
Affiliation:
Arcetri Astrophysical Observatory Largo Enrico Fermi 5 - 50125 Florence, Italy

Extract

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A slow evolving flaring loop has been observed by the UVSP, XRP and HXIS instruments on board SMM on June 10, 1980. Simultaneous radio observations from Toyokawa (Japan) are also available. The former instruments have an angular resolution ranging from 3“ to 30“ which allows the determination of the loop structure. The XRP:FCS rasters permit to analyze the flare only during three time intervals of about 10 minutes each.

Type
VIII. Solar Flares
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 454
Copyright
Copyright © Kluwer 1990 

References

REFERENCES

Chiuderi Drago, F. and Monsignori Fossi, B.C.: 1990, in preparation.Google Scholar