FLAMES OF COMPOUNDS OF CARBON AND HYDROGEN. 



427 



Table I. Observations of the Angle of the Prism. 



Series I. 



Series II. 



Total Number 

 ofObservations. 



Mean of all the 

 Observations. 



Number of 

 Observations. 



Mean of the Obser- 

 vations. 



Number of 

 Observations. 



Mean of the Obser* 

 vations. 



5 



60° 0' 15" 



3 



60° 0' 18" 



8 



60° 0' 16" 



Table II. Observations of the Solar Spectrum. 



Line of 

 Spectrum. 



Series I. 



Series II. 



Difference 

 of Means 

 I. and II. 



Collected Observations 

 or Minimum Deviations. 



Number of 

 Observa- 

 tions. 



Mean 

 I. 



Number of 

 Observa- 

 tions. 



Mean 

 II. 



Total Num- 

 ber of Ob- 

 servations. 



Mean of all the 

 Observations. 



A 



3 



47° 



20' 



27" 



3 



47° 20' 21" 



0' 6" 



6 



47° 20' 24" 



a 



2 



47 



29 



54 



4 



47 30 2 



8 



6 



47 29 59 



B 



2 



47 



39 



52 



3 



47 39 51 



1 



5 



47 39 51 



C 



2 



47 



50 



22 



3 



47 50 10 



12 



5 



47 50 12 



Pi* 











1 



48 50 





1 



48 50 



D 



2 



48 



18 



15 



4 



48 18 12 



3 



6 



48 18 13 



E 



2 



48 



55 



24 



4 



48 55 26 



2 



6 



48 55 25 



*t 



4 



49 



1 



45 



5 



49 1 44 



1 



9 



49 1 45 



\ 



2 



49 



2 



37 



1 



49 2 35 



2 



3 



49 2 36 



h 



2 



49 



2 



55 



3 



49 2 56 



1 



5 



49 2 55 



F 



2 



49 



29 



9 



3 



49 29 19 



10 



5 



49 29 15 



Pi* 







... 





4 



49 49 2 





4 



49 49 2 



G 



2 



50 



35 



2 



3 



50 35 5 



3 



5 



50 35 4 



H 



1 



51 



34 



50 



6 



51 34 43 



7 



7 



51 34 44 





Mean Temp. 

 Mean Barom 



of Prism, 53-3 F. 

 . . . 30-21 



Mean Temp. 

 Mean Temp. 

 Mean Barom 



of Prism, 64-2 F. 

 of Air, . 62-5 

 . . . . 29-98 







* Cj and Fj are used here to denote very strong lines adjacent to Fraunhofer's lines, C and F. 



t Fraunhofer denotes by 6 the two most refracted lines of a remarkable group, represented by three strong lines 

 in his map of the solar spectrum. I have here denoted these lines by 6, b v 6 2 , in the order of their refrangibility. 

 On 20th May, about 7 h 10 m P.M., when the sun was rather low in th e horizon, but free from clouds, I observed 

 with a power of 21, the line b 2 to be very finely but distinctly double, so that the group consists of four lines. 



VOL. XXI. PART III. 



5z 



I 



