SPECTRA OF SOME OF THE BRIGHTER STARS. 
691 
(3.) Table C.—Stars in which there is a continuous absorption in the ultra-violet 
or violet, extending to about G. In these stars the hydrogen lines are narrow. 
G-) 
In the spectra there are indications 
of dark flutings fading away 
towards the less refrangible end 
of the spectrum. 
(13.) 
There are no indications of flutings 
in the spectra. 
ft Andromedte 
1 ] Ceti 
a Ceti 
a Lyncis 
P Persei 
7 AndromedfB 
a Orionis (Betelgenx) 
a. Tanri (Aldebaran) 
/(, Geminornm 
cc Hydrse 
?. Virginia 
Ursee Majoris 
V Bootis 
ft Ursse Min oris 
h Ophinchi 
cc Serpentis 
K Ophinchi 
7 Draconis 
a Scorpii (Antares) 
)] Serpentis 
a Herculis 
0 ^ Cygni 
ft Pegasi 
e Cygni_ 
e Pegasi 
(4.) Table D.— Stars which are not included in any of the preceding Tables. 
y Cassiopeiae. 
Lyrae. 
P Cygni. 
Nova Aurigae. 
It will be seen, on reference to the Tables, that the bright-line stars of the Wolf- 
Rayet type, and the red stars of Group VI., have not yet been photographed at 
Kensington. All the stars of these types are very faint, and the dispersion hitherto 
employed has been too great to successfully cope with them. A larger aperture, with 
smaller dispersion, appears to be essential; and this has not yet been available. It is 
intended, however, to utilize the three-foot reflector for this work as soon as possible. 
All the stars of Table D show special features in their spectra, and will not be 
further considered in the present communication. 
V.—DISCUSSION OF STARS IN TABLE A. 
The stars included in this Table are characterised by the absence of any remark¬ 
able continuous absorption either in the violet or ultra-violet, and by the presence in 
their spectra of broad lines of hydrogen. As already shown, they may be conveniently 
classified into four sub-divisions, which we may now consider separately. The photo¬ 
graphs, which only show the lines of hydrogen, owing to small dispersion or defective 
definition, will be omitted from the discussion. 
4 T 2 
