

Ml. .1. K 



lines, the focus appears to be quite perfect through the whole length of 

 the spectrum. 



This suggests that the lens, which was a thin one, was under some 

 strain in its cell, and it accounts for the difficulty experienced in find- 

 ing the true focus. 



In the mid-eclipse photograph (No. 11) the bright lines are fairly 

 well defined at the extreme end of the spectrum, and they can lc 

 traced in this photograph to A. 3320. All the lines between A. 3340 

 and A. 3500 can be identified with those shown on the best plate ob- 

 tained in 1898. 



The following table gives the wave-lengths and identifications of 

 these lines as determined for the spectrum obtained in India. In 

 identifying the lines with the elements given in column 4, I received 

 great assistance from Mr. L. E. Jewell, who also supplied me with 

 a revised list of wave-length values for the solar lines given in 

 column 5. 



The intensities (column 2) are estimated as follows : 



Lines just visible but extremely faint 

 The strongest lines in the spectrum . 



= 

 = 10 



