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Heating the Quiet Corona by Nanoflares: Evidence and Problems

Published online by Cambridge University Press:  13 May 2016

A. O. Benz  and
S. Krucker
A. O. Benz
Affiliation:
Institute of Astronomy, ETH-Zentrum, CH-8092 Zürich, Switzerland
S. Krucker
Affiliation:
Space Sciences Laboratory, UCB, Berkeley CA 94720, USA

Abstract

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The content of coronal material in the quiet Sun is not constant as soft X-ray and high-temperature EUV line observations have shown. New material, probably heated and evaporated from the chromosphere is occasionally injected even in the faintest parts above the magnetic network cell interiors. Assuming that the smaller events follow the pattern of the well observed larger ones, we estimate the total energy input. Various recent analyses are compared and discussed. The results using similar EUV data from EIT/SOHO and TRACE basically agree on the power-law exponent when the same method is used. The most serious deviations are in the number of nanoflares per energy unit and time unit. It may be explained at least partially by different thresholds for flare detection.

Type
Session V: Coronal Heating and Solar Wind Acceleration
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 471 - 474
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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