The purpose of this paper is to report on some intensity measurements of the Fexm lines at 10 747 ~ and 10 798 ~ made during the total eclipse of 12 November, 1966. Infrared spectra were taken of the solar corona at a dispersion of 90 A~ per mm, using an RCA image converter and spectrograph aboard the NASA CV 990 aircraft off the coast of southern Brazil. The spectra have been reduced to equivalent width in terms of the coronal continuum and values derived for different points in the corona.
The observed equivalent widths of the lines lie in the range 10 to 30 N for the 10 747 line and 5 to 12 A_ for the 10 798 line. The ratio of these equivalent widths is found to vary from 2.3 in the inner corona to 6 at a point 1.36 solar radii from the center of the Sun.
The above results are discussed in terms of the excitation mechanisms involved in producing the lines. In particular, the results are compared with the recent theoretical calculations of Chevalier and Lambert, who are the first to include the effects of proton collisions in the excitation of the 3p2 3p levels of FexIII. Our observations are consistent with an electron density of 4 x 10 a in the inner corona; a value which compares favorably with those derived by other observers from the strength of the K continuum. These are, to our knowledge, the first eclipse observations of the infrared Fexm lines which indicate that proton collisions are important in the excitation of the coronal lines. The coronal abundance of iron is estimated from the equivalent width of the 10 747 line, and in common with other observers we find an overabundance as compared to the photospheric abundance by a factor of 10.