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On the magnetic field strength in the solar corona

Published online by Cambridge University Press:  14 March 2005

A.B. Delone ,
G.A. Porfir'eva ,
O.B. Smirnova  and
G.V. Yakunina
A.B. Delone
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij Prospect 13, Moscow 119992, Russia email: yakunina@sai.msu.ru
G.A. Porfir'eva
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij Prospect 13, Moscow 119992, Russia email: yakunina@sai.msu.ru
O.B. Smirnova
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij Prospect 13, Moscow 119992, Russia email: yakunina@sai.msu.ru
G.V. Yakunina
Affiliation:
Sternberg Astronomical Institute, Moscow State University, Universitetskij Prospect 13, Moscow 119992, Russia email: yakunina@sai.msu.ru
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Abstract

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On the base of the interferometric observations during the total solar eclipse on 11 August 1999 magnetic field strength in a coronal volume at the height of 10$^5$ km above the solar limb has been evaluated using an indirect method. A cold coronal emission (CCE), seen in the lines of $H_{\alpha}$ and K CaII, existed there. The conclusion is made that the magnetic field strength in this bulk, before the investigated CCE-region formed, was about 100-200 G.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 453 - 454
Copyright
© 2004 International Astronomical Union