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Number of Coronal Bright Points in Different Phases of the Solar Activity Cycle

Published online by Cambridge University Press:  14 March 2005

I. Sattarov ,
A.A. Pevtsov ,
N.V. Karachek  and
Ch.T. Sherdanov
I. Sattarov
Affiliation:
Tashkent State Pedagogical University, 103 Usif Xos-Hojib St., Tashkent 700100, Uzbekistan, email: isattar@astrin.uzsci.net
A.A. Pevtsov
Affiliation:
National Solar Observatory
Operated by the Association of Universities for Research in Astronomy (AURA, Inc) under cooperative agreement with the National Science Foundation (NSF).
, Sunspot, NM 88349, USA email: apevtsov@nso.edu
N.V. Karachek
Affiliation:
Tashkent State Pedagogical University, 103 Usif Xos-Hojib St., Tashkent 700100, Uzbekistan, email: isattar@astrin.uzsci.net
Ch.T. Sherdanov
Affiliation:
Tashkent State Pedagogical University, 103 Usif Xos-Hojib St., Tashkent 700100, Uzbekistan, email: isattar@astrin.uzsci.net Astronomical Institute AS of Uzbekistan, 33 Astronomicheskaya ul., Tashkent 700052, Uzbekistan email: chori@astrin,uzsci.net
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Abstract

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We present the preliminary results of study of the coronal bright points (BPs) using the SoHO/EIT data. We show that the number of BPs in quiet Sun areas does not vary between 1996 and 1997. In 1998 the BPs number (full disk) increases by about 20%.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Information

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 667 - 668
Copyright
© 2004 International Astronomical Union