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Properties of the magnetic field in the coronal holes in solar cycle 23

Published online by Cambridge University Press:  14 March 2005

K. S. Tavastsherna  and
A. G. Tlatov
K. S. Tavastsherna
Affiliation:
Pulkovo Observatory, St.Petersburg, Russia, email: tavast@gao.spb.ru
A. G. Tlatov
Affiliation:
Kislovodsk Solar Station of the Pulkovo Observatory, Russia, email: solar@narzan.ru
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Abstract

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The properties of the magnetic field in the coronal holes (CH) were considered during 1996-2002. The daily observations from the Kitt Peak observatory in the line HeI 10830Å were compiled. The measurement of the magnetic fields in the CH was carried out by comparing the data obtained from the Kitt Peak telescope and the magnetograms of SOHO/MDI. The dependence between the brightness of CH from intensity of the magnetic field and distributions of CH depending from the magnetic field and latitude were presented for minimum and maximum of the cycle. The latitude and the unipolarity degree of the magnetic field that influence on the brightness of the CH were examined. It was shown that the average magnetic field was 1-2G, the unipolarity degree of the magnetic field was 0.1-0.3 and brightness of the coronal holes increases with the average magnetic field. The latitude-time distributions of CH for different polarity were obtained.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. 301 - 302
Copyright
© 2004 International Astronomical Union