A series of spectrograms of the inner solar corona were obtained at the total solar eclipse of 30 May 1965 using a fast spectrograph with a circular slit that recorded the spectrum from 23000 to 29000 at all position angles around the limb simultaneously. In this paper absolute intensity is given as a function of position angle for the stronger lines and the continuum. In the coronal enhancement or condensation centered at heliocentric position angle 293 ~ absolute intensity is given for 34 forbidden emission lines and the continuum.
We present 30, 50, laO, and 200 ~m solar limb intensity profiles determined with arcsecond resolution from airborne observations of the occultation of the solar limb during the total eclipse of 1981 July 31. Two points of particular importance emerge: (1) The longerwavelength (100 and 200 ~m) limbs are significantly brighter than disk center. At 200 ~ the extreme limb is about 1.22 times the brightness of disk center. This is consistent with the 6000 K temperature-platE!au structure of the model chromospheres of Vernazza, Avrett, and
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