ATMOSPHERIC OZONE: ITS RELATION TO SOME 

 SOLAR AND TERRESTRIAL PHENOMENA 



By FREDERICK E. FOWLE' 



The reduction of the measurements of the output of radiation from 

 the sun obtained at the Smithsonian station on Table Mountain, 

 California (altitude 2.300 m.), encountered some difficulty which did 

 not seem to be present at the station at Montezuma, Chile (altitude 

 2.900 m.), in the southern hemisphere. Preliminary reductions showed 

 the presence of a direct relationship between the values obtained at 

 Table Mountain for the radiation from the sim and the amount of 

 ozone above that station. A yearly march present in the Table Moun- 

 tain solar results, together with other irregularities, were eliminated 

 when proper allowance was made for the amount of ozone al)ovc that 

 station. 



That ozone plays an important part in the interception of radiation 

 coming to us from the sun, especially at the violet end of the spectrum, 

 has been known for some time. It exerts absorption in the following 

 places in the spectrum : ' 



(1) A very strong band in the ultra-violet, 0.2300 to 0.3 lOO//. 

 with its maximum at 0.2550/x (the Hartley band). 



(2) A complicated group, extending roughly from 0.3100 to 

 0.3500JU. (the Huggins band). 



(3) A group in the yellow and red. 0.4500 to 0.6500/x (the 

 Chappuis band). 



(4) A band in the infra-red between 9 and i i//. 



* A preliminary report of this research was read at the 9th annual meeting 

 of the American Geophysical Union, April, 1928 (Ozone in the Northern and 

 Southern Hemispheres, Journ. Terr. Magn. and Atm. Electr. 33, 151, 1928). 



* Adapted, with alterations in the wave-lengths of the infra-red band, from 

 " The absorption of radiation in the ui)i)er atmosphere," C. Fabry, Proc. Phys. 

 .Soc. 39, I, 1926. 



Smithsonian Miscellaneous Collections, Vol. 81. No. 11 



