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140122 ||| eng |
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|a 9789400923317
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| 100 |
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|a Kundu, M. R.
|e [editor]
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| 245 |
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|a Energetic Phenomena on the Sun
|h Elektronische Ressource
|c edited by M. R. Kundu, B. Woodgate, E.J. Schmahl
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| 250 |
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|a 1st ed. 1989
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| 260 |
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|a Dordrecht
|b Springer Netherlands
|c 1989, 1989
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| 300 |
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|a XXVIII, 632 p
|b online resource
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|a 1: Preflare Activity -- 1.1 Introduction -- 1.2 Magnetohydrodynamic Instability. -- 1.3 Preflare Magnetic and Velocity Fields -- 1.4 Coronal Manifestations of Preflare Activity -- 1.5 References -- 2: Particle Acceleration -- 2.1 Introduction -- 2.2 Phenomena Associated with Mildly-Relativistic Electrons -- 2.3 Phenomena Associated with Ions and Relativistic Electrons in Solar Flares -- 2.4 Theoretical Studies Of Particle Acceleration -- 2.5 Achievements — Outstanding Questions -- 2.6 Acknowledgements -- 2.7 References -- 3: Impulsive Phase Transport -- 3.1 Introduction -- 3.2 Impulsive Phase Observations and their Interpretation -- 3.3 Theoretical Studies of Transport Processes -- 3.4 Summary -- 3.5 References -- 4: Chromospheric Explosions -- 4.1 Introduction -- 4.2 Crystal Spectrometer Experiments -- 4.3 Debate of Issue 1 -- 4.4 Debate of Issue 2 -- 4.5 Debate of Issue 3 -- 4.6 References -- 5: Flare Energetics -- 5.1 Introduction -- 5.2 Energetics of the Impulsive Phase -- 5.3 The Energetics of the Gradual Phase -- 5.4 Relationships among the Phases -- 5.5 Characterization of Total Flare Energy -- 5.6 Conclusions -- 5A. Flares Chosen for the Energetics Study -- 5B. A Review of Impulsive Phase Phenomena -- 5.7 Acknowledgements -- 5.8. References -- 6: Coronal Mass Ejections and Coronal Structures -- 6.1 Intrdocution -- 6.2 Observations -- 6.3 The Initiation of Coronal Mass Ejections -- 6.4 Modelling of Coronal Mass Ejections and Post-Flare Arches -- 6.5 Interplanetary Effects of Coronal Mass Ejections -- 6.6 The Slowly Varying Corona Near Solar Activity Maximum -- 6.6 Summary -- 6.7 Acknowledgements -- 6.8 References -- 7: Intercomparison of Numerical Models of Flaring Coronal Loops -- 7.1 Introduction -- 7.2 The Original Benchmark Problem -- 7.3 Initial Solution Comparisons -- 7.4 Final Benchmark Problem andSolution Comparison -- 7.5 Conclusions -- 7.6 References -- SMM Participants
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| 653 |
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|a Astrophysics
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| 700 |
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|a Woodgate, B.
|e [editor]
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| 700 |
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|a Schmahl, E.J.
|e [editor]
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| 041 |
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|a eng
|2 ISO 639-2
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| 989 |
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|b SBA
|a Springer Book Archives -2004
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| 490 |
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|a Astrophysics and Space Science Library
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| 028 |
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|a 10.1007/978-94-009-2331-7
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| 856 |
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|u https://doi.org/10.1007/978-94-009-2331-7?nosfx=y
|x Verlag
|3 Volltext
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|a 523.01
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| 520 |
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|a This publication is a result of three meetings, each 5 days long, held at the Goddard Space Flight Center on January 24-28, 1983, June 8-14, 1983, and February 13-17, 1984. The meetings were held in the interim between the full operations of the Solar Maximum Mission (SMM) in 1980, and the renewed operations after its repair in orbit in April 1984. Their general objectives were as follows: o Synthesize flare studies after three years of SMM data analysis. Many analyses of individual flares and individual phenomena, often jointly across many data sources had been published, but a need existed for a broader synthesis and updating of our understanding of solar flares since the Skylab Flare Workshops held several years earlier. o Encourage a broader participation in the SMM data anlysis and combine this more fully with theory and other data sources--data obtained with other spacecraft such as the HINOTORI, P78-1, and ISEE-3 spacecrafts, and with the Very Large Array (VLA) and many other ground-based instruments. Many coordinated data sets, unprecedented in their breadth of coverage and multiplicity of sources, had been obtained within the structure of the Solar Maximum Year (SMY). o Stimulate joint studies, and publication in the general scientific literature. The intended primary benefit was for informal collaborations to be started or broadened at the Workshops with subsequent publications. o Provide a special publication resulting from this Workshop. o Provide a starting point of understanding for planning renewed full observations with the repaired SMM.
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