Various instruments were used to observe the solar corona and prominences near or at the time of solar eclipse, 22 July 1990. The white-light solar corona pictures were observed nearly up to R = 3 (solar radii) with the Úpice Observatory eclipse team at Markovo. Both emission line intensities (the green and red corona) and prominences were obtained at Lomnický Peak coronal station. These data sets are used to identify active coronal regions. A large coronal hole was observed above the south pole and extending nearly up to R = 2.5. Large-scale structure of the white-light corona is very complicated. There are many streamers nearly equally distributed around the whole Sun (except the south pole). Several streamers above the solar surface are not extended radially with
their height. In the NE quadrant 4 voids are clearly seen at the height of about R = 2. A slight excess of the white light corona is in favor of the west limb, however, the emission corona has an opposite meaning. Green and red corona, similarly as prominences, showed rapid changes in active regions over the eclipse period, however, any CME was not directly observed. The integral brightness of the 22 July 1990 white-light corona was estimated as JK = 1.32 x 10~6 and the ellipticity, a + b = 0.04. The white-light corona was nearly a maximum type.
The paper shows that the deviations of the plane of polarisation from the normal direction found by us are due to scattering of the polarised lights of the corona on ice-crystals in high layers of troposphere. Nevertheless, the deviations in the equatorial regions can hardly be explained in this way, and they seem to be real. and Součástí článku jsou fotografie s popisky v angličtině (nestránkováno)