Titlebook: Energetic Phenomena on the Sun; M. R. Kundu,B. Woodgate,E. J. Schmahl Book 1989 Springer Science+Business Media Dordrecht 1989 Corona.Plan

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https://doi.org/10.1007/978-3-642-99076-2 kinds of activity. The launch of the SMM presented an opportunity to study the low and intermediate corona from space with multiple instruments for protracted periods of time. This opportunity had been lacking for years, and it was enthusiastically awaited by those interested in coronal studies. Th

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https://doi.org/10.1007/978-3-642-98948-3egime, has demonstrated convincingly that the corona is pervaded at all times by loop-shaped features that appear to be closely aligned with ambient magnetic field lines. This structuring is most strikingly evident in solar active regions. Together with photospheric magnetograms, the orientations of

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https://doi.org/10.1007/978-94-009-2331-7Corona; Planet; Solar flare; solar; solar activity

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Particle Acceleration,he Sun during a solar flare is inferred from the observed electromagnetic radiation resulting from the interaction of the energized particles with the ambient plasma and/or the magnetic field as well as from direct particle observations in interplanetary space. In this chapter we compile data from t

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Impulsive Phase Transport,on and to subsequently release it on a sufficiently short time scale. Satisfactory solution of the solar flare problem will require at least two achievements by the solar physics community: first, convincing theoretical demonstration that one or more mechanisms of energy storage and release can occu

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Obstruction

Flare Energetics,rgy within a flare. To achieve this goal, we chose five flares in 1980 that were well observed with instruments on the Solar Maximum Mission, and with other space-borne and ground-based instruments. The events were chosen to represent various types of flares. Details of the observations available fo

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Intercomparison of Numerical Models of Flaring Coronal Loops,egime, has demonstrated convincingly that the corona is pervaded at all times by loop-shaped features that appear to be closely aligned with ambient magnetic field lines. This structuring is most strikingly evident in solar active regions. Together with photospheric magnetograms, the orientations of