Eh. I. Tetruashvili

The results of statistical analysis of the coronal profiles above the solar active regions

In order to establish some regularities or variations in the distribution of widths and intensities of the coronal line profiles λ 5303 and λ 6374 depending upon the solar activity, a statistical analysis was made for more than 3000 profiles (the data covering the period 1966–1972).The following results obtained:(1)The distribution of coronal line profile widths changes depending upon the solar activity phase.(2)The character of the relation between the intensities and widths varies with variation of the solar activity phase.

On 5694 Å coronal line observations

Coronal yellow line emission was observed by the Lyot coronagraph at the Abastumani Astrophysical Observatory. Line intensity is I = 45 erg cm−2 s−1 sr−1 Å−1, its half-width Δλ = 1.3 Å, electronconcentration ne = 7.5 × 109 cm−3.

The results of coronal investigation at the September 22, 1968 solar eclipse

The 1968 Abastumani Astrophysical Observatory Solar Eclipse Expedition obtained photographic records of the polarization and intensity of the solar corona on September 22 from a site of the South Urals (Western Siberia). A photometric study of the corona was carried out. Polarization has been computed both in a total corona and in some of its streamers. The coronal intensity Ik and IF components are separated. Electron concentrations and temperatures are computed.

On the formations connected with the limb flare of November 6, 1979

We analyzed the observation data obtained at Abastumani astrophysical observatory in the form of spectrograms and filtergrams of formations associated with the November 6, 1979 limb flare. We studied the system of flare loops, the late stage of the bright flare loop development, and postflare coronal loops obtained inHα and coronal lines. The physical parameters of the structures observed as well as their dimensions and mutual locations are determined. The Doppler velocities at different altitudes are measured and the prevailing upward direction of the matter motion in the flare loops is revealed.