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What Can Be Learned About Competing Acceleration Models from Multiwavelength Observations?

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Energy Conversion and Particle Acceleration in the Solar Corona

Part of the book series: Lecture Notes in Physics ((LNP,volume 612))

Abstract

We review the available evidence from various wavelength ranges, alone and in combination, bearing on solar particle acceleration. Radio, X-ray and γ-ray observations yield direct information on ion and electron acceleration at the Sun. We describe the main spectral features in the X/γ domain, outline the means by which they yield information on accelerated particles, and summarise results obtained using them on numbers and energies of flare fast ions and electrons. Relative numbers and energy content of electrons and ions may vary from flare to flare, and in the course of a single event. In general, both electronic and ionic species appear to embody significant fractions of the total flare energy and either can be dominant, although there is great uncertainty over accelerated particle minimum energies. Rapid fluctuations in X/γ- rays point to a fragmented accelerator, acting on timescales of 100 ms or less, even after particle transport effects have been considered. Millimeter wave observations also reveal spatial fragmentation. Together with distributions of overall event size, such fragmentation suggests a scale-invariant energy release process, such as would occur in a state of Self-Organised Criticality. There is good evidence from X/γ and cm/mm observations for hardening of the electron distribution towards the MeV energy range. Intercomparisons of X/γ rays and cm/mm wave observations emphasise the importance of MeV energy range electrons in the latter. ‘Electron-rich’ events, characterised by a hard electron population extending to relativistic energies, may occur during individual flares. Existing instrumental capabilities mean that the absence of γ-ray lines does not rule out significant, simultaneous ion acceleration. Radio observations indicate these spectral changes are associated with changes in spatial structure. Spatially resolved radio observations indicate that primary particle acceleration takes place moderately high in the corona (107 to 108 m), and have recently been made to yield information on accelerated electron pitch angle distribution. Throughout, we emphasise questions on which the unprecedented capabilities of the RHESSI mission will shed new light.

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  1. LESIA, Observatoire de Paris, Section d’Astrophysique de Meudon, 92195, Meudon-Cedex, France

    Nicole Vilmer

  2. Department of Adult & Continuing Education, University of Glasgow, G 31LP, Glasgow, UK

    Alexander L. MacKinnon

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  1. Observatoire de Paris, Section de Meudon, LESIA, 5, place Jules Janssen, 92195, Meudon Principal Cedex, France

    Karl-Ludwig Klein

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© 2003 Springer-Verlag Berlin Heidelberg

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Vilmer, N., MacKinnon, A.L. (2003). What Can Be Learned About Competing Acceleration Models from Multiwavelength Observations?. In: Klein, KL. (eds) Energy Conversion and Particle Acceleration in the Solar Corona. Lecture Notes in Physics, vol 612. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-36242-8_9

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  • DOI: https://doi.org/10.1007/3-540-36242-8_9

  • Publisher Name: Springer, Berlin, Heidelberg

  • Print ISBN: 978-3-540-00275-8

  • Online ISBN: 978-3-540-36242-5

  • eBook Packages: Springer Book Archive

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