With the purpose of detecting periodic oscillations or waves in a quiescent prominence, temporal variations ofa CaII K line profile have been studied. The most conspicuous phenomenon found here is the fact that the edge of the prominence showed, over some 20000 km along the spectrograph-s/it, periodic velocity fluctuations of nearly the same phase with periods of 210-240 s and with an amplitude of up to + 2 km s -1. At other portions, several different periods of peaks (160-400 s) can also be seen in the power spectra, but less distinctly. As to the intensity and the line width, however, no periodic variations have been detected.

A technique developed for analysing line profiles with both speed and high accuracy was used to study the physical conditions of a coronal formation near a quiescent prominence. Detailed analyses of five coronal lines (Fe XlV ),5303, Fe x ~,6374, Ni xv 26702, Fe xv 27059, and Fe x127892) provided total intensities, Doppler width temperatures, ionization temperatures, and velocities. Dissimilar spatial fluctuations in intensity are obvious for ions grouped according to (low vs high) ionization potentials. The intensity of the green line shows a local minimum around the observed quiescent prominence; a corresponding but much more diffuse pattern is visible in the red line intensity.Large differences are observed in temperatures derived by different means. In particular,, and ]~e(XI/X)= = 1.2 • 106K. The differences between Te(xv/xlv) and Te(x~/x) are taken as direct evidence of temperature inhomogeneity. One can thus put little significance in Te(xlv/x). TD (25303) and Te(xv/xIv) fluctuate nearly in parallel at each slit height, with a weak local minimum evident around the prominence. The discrepancy between these two can be removed if a non-thermal turbulent motion of 6-16 km s -s is assumed. Variations with height of both TD(25303) and Te(xv/xIv) suggest that the coronal temperature maximum is located no more than 15000 km above the top of spicules.A negative gradient of about 6 deg km 1 is found in the height variation of TD(25303). The height variation of the green line wavelength shows that the majority of coronal material in this region is flowing from west to east on the Sun, with the highest velocity of 12 km s -1 found at the lowest heights. This motion is in the same sense as that of the nearby coronal rain, as determined both from the spectra and wavelength-shifted Ha filtergrams. Superposed on the above flow is a systematic velocity field of up to • 5 km s -1. This field similarly reaches maximum amplitudes at lowest heights showing a local maximum around the prominence.

Spectrographic observations of the flash spectrum were made by the Kwasan Observatory at the total solar eclipse on 7 March, 1970. The integrated intensities of Fexiv ,~ 5303, Fex ~ 6374, and the continuum were measured on the spectrograms as a function of height above the Sun's limb. It was found that a large amount of emission in the coronal lines originates in the interspicular regions of the chromosphere. Analysis of the data yielded that the interspicular regions consist of coronal material of Te= 1.6 x 106-1.2 x 106 and log Ne=8.5-9.5, and that a decrease in T, and an increase in N~ occur with decreasing height.

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Slitless flash spectrograms in heights below 8000 km above the solar limb were obtained by the