Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-29T15:10:09.101Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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 

References

Aschwanden, M.J. et al., 2000, ApJ, 535, 1047.CrossRefGoogle Scholar
Benz, A.O., Krucker, S. 1998, Solar Phys., 182, 349.CrossRefGoogle Scholar
Benz, A.O., Krucker, S., 1999, ESA SP-448, 547.Google Scholar
Berghmans, D., Clette, F., Moses, D., 1998, Astron. Astrophys., 336, 1039.Google Scholar
Berghmans, D., Clette, F., 1999, Solar Phys., 186, 207.CrossRefGoogle Scholar
Brown, J.C., Krucker, S., Güdel, M., Benz, A.O., 2000, Astron. Astrophys., 359, 1185.Google Scholar
Krucker, S., Benz, A.O., Acton, L.W., Bastian, T.S., 1997, ApJ, 488, 499.CrossRefGoogle Scholar
Krucker, S., Benz, A.O., 1998, ApJ, 501, L213.CrossRefGoogle Scholar
Krucker, S., Benz, A.O., 2000, Solar Phys. 191, 343.CrossRefGoogle Scholar
Parnell, C.E., Jupp, P.E., 2000, ApJ, 529, 554.CrossRefGoogle Scholar
Shimizu, T., 1995, PASJ 47, 251.Google Scholar