Abstract
heights. The maximum brightness of the corona was observed in the equatorial zone in the solar minimum. The drifts of coronal intensity were observed in direction to the poles in the beginning of solar cycle. The maximum brightness of high-latitude corona was observed during the polar magnetic field reversal of the Sun in 1999‐2001. The drifts of low coronal brightness were observed in the opposite direction from high latitudes to the equator after polar magnetic field reversal. The angles of deviation from radial direction of coronal streamers were determined on daily coronal images. It was found that coronal streamers were inclined on the whole to the equator during 1996.5‐1999.5, although after 1999.5 the streamers were inclined to the poles. The angles of nonradial direction of the streamers reached about 10 ‐15 . The longitudinal distribution of coronal brightness at various heights was considered. It was compared with heliosphere neutral layer and with drift of filament bands in an epoch of polar magnetic field reversal of the Sun. INDEX TERMS: 7509 Solar Physics, Astrophysics, and Astronomy: Corona; 7524 Solar Physics, Astrophysics, and Astronomy: Magnetic fields; 7536 Solar Physics, Astrophysics, and Astronomy: Solar activity cycle; KEYWORDS: Solar corona; coronal rays; coronal observations.
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