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General aspects of the dynamics of capillary rise are considered with references to extant theories. A stroboscopic method used to study the rise of a liquid in a capillary tube is discussed. Tables are presented showing the observed heights at various times during the rise for the liquids—water, ethyl alcohol, and glycol in each of three capillaries of different diameters.

299were made using a water-cooled hollow cathode source, operated at about 1-mm pressure of argon. The resonance lines were investigated first with a thirty-foot grating in the second order, and with iron and krypton comparison spectra. Components a and d of the 4101A line were resolved by this instrument while components b and c were not. The 4511A line complex appeared as two components. A further check was made with the

Additional observations of He II (304 &) and Si xI (303 ~) were obtained from a high resolution rocket spectrograph flown on 30 August, 1973 and 20 January, 1975. The profile of the He ri (304 ~) line is everywhere clearly non-gaussian across the solar disk, except in bright active areas. Near the limb, the profile is distinctly reversed. The profile of the Si xr (303 *) line is essentially gaussian for all regions across the solar disk. Measurements of the He II/Si xr intensity ratio indicate that the average value of this ratio across the disk depends markedly on solar activity, being about 10:1 for a moderate level of activity and 30 : 1 for a quiet Sun.