RESULTS OF OBSERVATIONS OF THE CORONAL SPECTRUM OF 19 JUNE 1936.
Solar research note,
SACRAMENTO PEAK OBSERVATORY SUNSPOT N MEX
Pagination or Media Count:
Chiefly, the results of spectrophotometric study of emission lines in the spectrum of the inner corona are cited 1 The total intensity of emission lines changes from one coronal region to another and from eclipse to eclipse 2 a comparison of spectrophotometric measurements of spectra for 1929 and 1936 reveals considerable difference with respect to intensity of emission lines for example 5303, 6374, 3801, 3987 and 4086 3 the decrease in intensity of emission lines with distance from the edge of the disk is not proportional to the corresponding decrease of intensity of the continuous spectrum gradients are considerably higher for lines, with the exception probably, of 4231 4 the observed deviation in curves of intensity changes in lines and in the continuous spectrum with distance from the edge of the disk should be attributed, first of all, to local effects 5 the validity of the observed retardation in the growth of intensity of emission lines, or even the decrease of intensity within limits 0-1, is doubtful. One can suspect the presence of a decrease in intensity for distances less than 0.5 only on the basis of indirect reasoning 6 a change in the intensity of the continuous spectrum within 1-6 does not show appreciable dependence on wave length 7 the density of matter responsible for the continuous spectrum electrons changes from 1.6 X 10 to the 8th power to 0.3 X 10 to the 8th power within 1.5--5.5. The corresponding change of particles responsible for emission lines is 6-7 times greater. Author