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Waves in the Solar Corona

Published online by Cambridge University Press:  26 May 2016

Eckart Marsch
Eckart Marsch*
Affiliation:
Max-Planck-Institut für Aeronomie, 37191 Katlenburg-Lindau, Germany

Abstract

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Waves at all scales, ranging in wavelength from the size of a loop (fraction of a solar radius) down to the gyroradii of coronal ions (about hundred meters), are believed to play a key role in the transport of mechanical energy from the chromosphere to the Sun's corona and wind, and through the dissipation of wave energy in the heating and sustaining of the solar corona. A concise review of new observations and theories of waves in the magnetically confined (loops) as well as open (holes) corona is given. Evidence obtained from spectroscopy of lines emitted by coronal ions points to cyclotron resonance absorption as a possible cause of the observed emission-line broadenings. Novel remote-sensing solar observations reveal low-frequency loop oscillations as expected from MHD theory, which appear to be excited by magnetic activity in connection with flares and to be strongly damped. Kinetic models of the corona indicate the importance of wave-particle interactions that hold the key to understand ion acceleration and heating by high-frequency waves.

Type
Part 9: Heating of Solar and Stellar Coronae
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 449 - 460
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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