THE SPECTEA OE SOME OE THE FIXED STAES. 
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(5) Iron. — The lines in the spectrum of this metal are very numerous, but not remark- 
able 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 coin- 
cided with four in the spectrum of the star. 
(8) Antimony. — Three of the lines in the spectrum of antimony were observed to coin- 
cide 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 all the spectra of the elements above 
enumerated do not possess corresponding lines in the star-spectrum. Comparisons of 
this kind are extremely 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. nitrogen, cobalt, tin, lead, cad- 
mium, lithium, and barium. No coincidence 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 XI.). — The light of this star has a decided orange 
tinge. None of the stars which we have examined exhibits a more complex or remark- 
able 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 therefore not inserted them in the Table or the dia- 
gram. We have measured the position of about eighty lines in the brighter portions 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 from 1145 
to 1170, and from 1280 to 1300. A similar shaded band commences at 1420, and 
another at 1557. 
The spectra obtained from sixteen elementary bodies were observed simultaneously 
with the spectrum of a Orionis. In five of these, viz. sodium, magnesium, calcium, iron, 
and bismuth, lines corresponding with certain stellar lines were found to exist. 
(1) Sodium. — The lines coincident with D are fainter in this star than in Aldebaran. 
(2) Magnesium. — Decided group of three stellar lines coincident with the group at b. 
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