SOLAK ECLIPSE, MAY 6, 1883. 



77 



Computation of relative solar intensities — (Jontimied. 

 MAY 2. 



MAY 3. 



p. M. 

 1.15 

 1.30 

 2.00 

 3.00 

 3.15 



36.7 

 37.1 



36.8 

 36.2 

 35.4 



33.1 

 33.2 

 33.1 

 32.9 

 32.2 



MAY 6. 



29.4 

 29.4 

 29.4 

 29.0 

 29.0 



7.3 

 7.7 

 7.4 

 7.2 

 6.4 



3.7 

 3.8 

 3.7 

 3.9 

 3.2 



10.8 

 11.7 

 11.0 

 10.4 

 9.8 



All ex;imiiiatioii of the values of tlie inteusity giveu in the last coluiiiii shows many iiregu- 

 laiities. This is not due to the effect of passing clouds, as in the former methods, for the thermom- 

 eters recover quickly their former condition after the clouds have passed, but to changes in the 

 velocity of the wind. The method is confessedly approximate, since the least increase in the force 

 of the wind which blows on the bulbs, or the least decrease, changes the effect of convection 

 and so produces discordancies in the observations. The values obtained ai'e therefore more of 

 interest for comparison than for their intrinsic merit. 



4. COMPAEiaON OF THE KELATIYE INTENSITIES. 



It remains to make a comparison between the intensities obtained by the three methods in 

 use. For this purpose they must be reduced to a common scale. The intensity at 12.00 on May 1 



