420 Mr. W. Huggins and Dr. W. A. Miller on the 



(5) Iron. — The lines in the spectrum of this metal are very- 

 numerous, but not remarkable for intensity. There was a 

 double line corresponding to E in the solar spectrum, and three 

 other more refrangible well-marked lines coincident with lines in 

 the star. 



(6) Bismuth. — Four strong lines in the spectrum of this metal 

 coincided with four in the star-spectrum. 



(7) Tellurium. — In the spectrum of this metal also four of 

 the strongest lines coincided with four in the spectrum of the 

 star. 



(8) Antimony. — Three of the lines in the spectrum of anti- 

 mony were observed to coincide with stellar lines. 



(9) Mercury. — Four of the brightest lines in the mercury- 

 spectrum correspond in position with four lines of the star. 



It must not be supposed that other lines in the spectra of all 

 the elements above enumerated do not possess corresponding 

 lines in the star-spectrum. Comparisons of this kind are ex- 

 tremely fatiguing to the eye, and are necessarily limited to the 

 stronger lines of each spectrum. In no case, in the instances 

 above enumerated, did we find any strong line in the metallic 

 spectrum wanting in the star-spectrum, in those parts where the 

 comparison could be satisfactorily instituted. 



Seven other elements were compared with this star, viz. nitro- 

 gen, cobalt, tin, lead, cadmium, lithium, and barium. INo coin- 

 cidence was observed. With nitrogen three strong double lines 

 were compared, with cobalt one strong single line and. a double 

 line, with tin five lines, with lead two strong lines, with cadmium 

 three lines, with barium two of the strongest in the green, and 

 with lithium the line in the orange, but were found to be without 

 any strong lines in the star-spectrum corresponding with them. 

 The positions of these several lines relatively to the star-spectrum 

 are given in the diagram. 



12. u Orionis (Betelgeux) (Plate VI.). — The light of this star 

 has a decided orange tinge. None of the stars which we have 

 examined exhibits a more complex or remarkable spectrum than 

 this. Strong groups of lines are visible, especially in the red, 

 the green, and the blue portions. In the blue comparatively few 

 of these lines have been measured with accuracy ; we have there- 

 fore not inserted them in the*Table or the diagram. We have 

 measured the position of about eighty lines in the brighter por- 

 tions of this spectrum. 



In the interval between the divisions 890 and 920 of the scale 

 adopted in the diagram, is a shading as of fine lines. A fainter 

 shading of the same character is observed between 990 and 1010, 

 also from 1050 to 1069. A stronger similar shading occurs 



