The faint emission of hydrogen, helium and metals in the corona which appeared near an active prominence is studied. The calculations showed that the temperature of the emission region is in the limits from 10000 K to 30000 K and the electron density is between 109-10 x~ cm -3, respectively.

The spectrum of the solar corona obtained during the eclipse of 7 March, 1970 has been studied. From the analysis of the line halfwidths it is concluded that the emission of coronal lines of various groups arises in different volumes of the corona. The lines 15303 and 14231 are analyzed in detail and by the use of the equations of excitation and ionization balance. The distribution of electron temperature Te and density n~ vs height in the solar corona has been found. The usually adopted n~ and % are noticeably less than those values obtained in present analysis. This discrepancy may be due to the fact that the considered area of the corona seems to be in an unusual condition.