= 
Huggins and Miller on the Spectrum of a new Star. 391 
at small eer as far as the spec etrum can be tr 
n of the gaseous spectrum.—A bright Lina, much more 
brilliant ro the part of the continuous spectrum upon which 
it falls, occupies a position which several measures make to be 
coincident with Fraunhofer’s F.* At rather more than one-fourth 
of the distance which separates F and G, a second and less bril- 
liant line was seen. Botti these lines were narrow and sharply 
defined. Beyond these lines, and at a distance a little more 
than one- thaed: of that which separates the second bright line 
from the strongest bright one, a third bright line was observed. 
€ appearance of this line suggested that it was either double 
of the spectrum, Serod: a line brighter than he 
normal relative brillianey’ of this part of the spectrum. ‘h 
brightness of this line, however, was not nearly so marked in 
proportion to that of the part of the spectrum i it occurs, 
as was that of the lines in the green and blue.” 
General conclusions.—It is difficult to imagine the present phys- 
ical constitution of this remarkable object. There must be a 
photosphere of matter in the solid or liquid state emitting light 
of all refrangibilities. Surrounding this must exist also an at- 
: uced by taking the induction-spark 
through the thes soe a Smal lion a the teen imultaneously with 
the beioht lines of the star. The brightest line coincided with the middle Tf the 
expanded line of hydrogen which corresponds to Fraunhofer’s F. On pie net 
the faintness of the red end se = rum, when the amount of di 
sary for these observations w: Sved th the exact eoincidence of the ‘aie tn ie 
part of the spectrum with the ie line of Sparores, though extremely probable, 
was not determin oe aaa equal certainty. 
pe estar were observed again on the 17th, the 19th, the ae 
and the 23d. On in evenings no important alteration oe 
lith an e t of 
veni 
than on the 16th, the ved bright line ine appeared a ond brighter rohateity raed 
green and blue bright lines. On the 19th and 21st the absorption lines about 6 
were stronger than on the 16th. From the 16th the continuous spectrum n- 
more give he gaseous spectrum, so than on the 23d, 
though the s as a whole was faint, the bright lines were brilliant when 
compared with the continuous spectrum. eae 
