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Modelling of Solar Coronal Loops

Published online by Cambridge University Press:  30 March 2016

C. Jordan
C. Jordan*
Affiliation:
Department of Physics(Theoretical Physics) University of Oxford1, Keble Road, Oxford 0X1 3NP, U.K.

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Modelling of coronal active regions in terms of loop structures began around 1974 (see Jordan 1975) and was stimulated by images of the corona in X-rays and the uv, obtained from rocket flights. Vaiana was a pioneer in this field (see Vaiana et al. 1973). The Skylab missions provided a fuller range of imaging and spectroscopic observations, and much of the available information is still based on these data (see Orrall 1981). Since 1975 a very large number of papers have been published on the various aspects of loop structure, heating and stability (see review by Mewe 1991). Here I can mention only a few points concerning the relation between observable parameters and the energy balance and heating requirements of active region loops.

Type
Joint Commission Meetings
Information
Highlights of Astronomy , Volume 9: Highlights of Astronomy. As presented at the XXIst General Assembly of the IAU, 1991 , 1992 , pp. 661 - 662
Copyright
Copyright © Kluwer 1992

References

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