V—2 ROCKETS—KRAUSE 
all observed minima are blends from 
two or more closely spaced lines, but 
the principal contributors have, in 
many cases, been identified. Of par- 
ticular interest was the appearance of 
the Mg II doublet at 2795 and 2802 A. 
as bright emission lines in the center of 
a broad absorption region created by 
the same pair (25). 
EXPLORER IL 
INDIRECT 
ALTITUDE (KM) 
VERTICAL OZONE DISTRIBUTION 
WHITE SANDS, N.M. OCT.10,1946 
TOTAL 03 2.7MM_ S.T.P. 
199 
The effect of the absorption of ozone 
can be clearly seen by noting the 
absorption band in the region of 
2300 to 2800 A. below 55 km. ‘The 
vertical distribution of ozone on this 
flight is shown in figure 6 (27). The 
results of the 1936 Explorer IJ balloon 
flight (5) are shown for comparison. 
The balloon data above 22 km. are 
PRELIMINARY 
NRL 
DIRECT 
Be 
02 0 
3 0 
4 
CM Oz /KM 
Figure 6.—Vertical ozone distribution. 
The double layer is rather unusual but has been 
reported previously. 
3. Line shapes—Line widths and 
intensities are important in determin- 
ing excitation conditions in the sun, 
and necessary to an understanding of 
the fundamental processes occurring 
there. Considerable information on 
this subject is contained in the spectra. 
Full analysis and evaluation of condi- 
tions in the sun will require another 
year or more of intensive work. 
4. Ozone—The variations of the 
spectra with altitude for the October 
10 flight are shown in plate 5, figure 2. 
817369—49—_15 
based on an indirect method and lack 
the inherent accuracy of the direct 
method employed from the rocket. 
Further data are required to determine 
whether the disagreement at high 
altitudes is due to a real variation in 
the ozone or to experimental error. 
The lower maximum is known to be 
present on days when the total ozone 
content of the atmosphere is abnor- 
mally high (28). 
5. Sky brightness—Some data in the 
ultraviolet are available. The experi- 
