SOLAR ECLIPSE, MAY 6, 1883. 



85 



The corresponding values of p are 0.735 and"t).751, respectively. Early morning and evening 

 observations are wanting on April 29 and May 3, and wben this is the case values of A between 

 2.2 and 2.0 will satisfy the observations with nearly equal accuracy. It seemed best, therefore, 

 to adopt for the final value that obtaiue<l on the dates April 30, May 1 and 2, viz : 



A = 2.322 

 Reducing to the sun's mean distance we have finally : 



A = 2.285 



RADIATION OBSERVATIONS DURING- THE ECLIPSE. 



There has already been given a detailed account of the observations of solar radiation made 

 from day to day, and the methods of reduction by which values of the solar intensity were 

 obtained. On the day of the eclipse, readings were made from 10.00 a. m. to 1.15 p. m. by Seaman 

 J. C. Harold, of the Hartford. They were made every two minutes from 11.30 to 11.40, in which 

 interval the period of totality was included, and every five minutes at other times. Flying clouds 

 concealed the sun at occasional intervals, and therebv affected the observations to some extent 

 but the results are quite satisfactory. The instruments used were conjugate thermometers Nos. 

 1 and 3, Violle's bulbs with black-bulb thermometers Nos. 742 and 751,. and ordinary black 

 and bright bulb thermometers Nos. 1137 and 1136. The observer made readings to the nearest 

 half degree. The observations in detail are given in connection with those of other days. 



The design of the observations was to determine what proportion of heat received by the 

 earth was cut ofl' by the concealing of the sun, and also the shape of the curve representing the 

 varying solar intensity. The necessary computations were made on the plan already fully 

 explained. The following table contains the results of the computation; the air temperatures 

 were interpolated from the curve previously given. 



Solar intensities during eclipse. 



