Investigation of the white light coronal structure during the total solar eclipse on March 29, 2006

Details Investigation of the white light coronal structure during the total solar eclipse on March 29, 2006 Investigation of the white light coronal structure during the total solar eclipse on March 29, 2006

Feb 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jastp..70..414s&link_type=abstract

Journal of Atmospheric and Solar-Terrestrial Physics, vol. 70, issue 2-4, pp. 414-419

Physics

2

Total Solar Eclipse, Corona, Photometry

Scientific paper

Results from photographic observations of the white light solar corona conducted during the total phase of the total solar eclipse on March 29, 2006 in Manavgat, Turkey are shown in this work. Spectroscopic study of the green 530.3 nm line of Fe XIV in the corona of the Sun has also been made. The spectrograph was designed by specialists from the STIL-BAS "Acad. D. Mishev", Stara Zagora Department, Bulgaria; the Lebedev Physical Institute, Moscow, Russia; and the Yuri Gagarin Public Astronomical Observatory, Stara Zagora, Bulgaria. It has been found that the axis of symmetry of the "helmet"-type streamers is tilted towards the solar equator and the deviations from a radial direction in the western hemisphere are greater than those in the eastern one (21°/8°). The solar corona flattening is [epsilon]=0.098, which corresponds to an intermediate (before the minimum) type of corona. We have obtained that the solar cycle phase is [Phi]=0.17 for the 2006 TSE. White light corona is asymmetric, in contrast to solar corona observed during the August 11, 1999 total solar eclipse.

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