ON STAR STREAMING, 265 
What may be the cause ? 
Light will be thrown thereon if more ample data confirm what I 
found from my scanty store, apparently even more decisively than 
Campbell's phenomenon, viz., that these stars also lead to a very small 
velocity of the solar system. 
For this would make us conclude that the stars nearest to the solar 
system partly participate ih its motion. The ccnclusion is strengthened 
by various considerations, into which time does not allow me to enter now. 
On the other hand there were very serious, though perhaps not 
insuperable, objections which would rather make us seek an explanation 
in quite another quarter, and which at least comp<! us to wait for further 
information. 
But, whatever may be the cause of the phenomenon, whether it be 
cosmical or even only instrumental, we miust expect that the spectroscopic 
observations of the bright stars will show the phenomenon of the star- 
streams less strongly than will the observations of fainter stars ; and as 
our list is made up in great part of such bright objects we must expect to 
find their influence show in a somewhat less marked degree than we 
would be led to imagine from the considerations of this paper, which are 
based on the whole of the stars down to the ninth magnitude. 
Now this is just what we find to be the case. 
1 find, arranging in order of the distances from the nearest of the 
vertices :— 
— Real velooity in the line of sight 
iwc eta a | ai S i im 
| Mean distance from C | Number of : 
Mth rest verted Obs. veloc. | afaik | Theor. | 0°827 x Theor. | 
SS ee sessile ak Waatealedl Sats: aero | 
| 31 17°37 CAD)e Lajipl Laws BERG oS eAlT jLckR99( 4. | 
| 59 13:78 (39) | 15-98 13 22 ! 
79 11:16 (45) 13°15 10°87 
Mean 1425 | (124) 17-23 14-25 
Amplitude 6-21 
The phenomenon is clearly shown. The observed numbers, however, 
are only nearly 83 per cent. and the observed amplitude but 72 per cent. 
of the theoretical value. 
A small but independent contribution is furnished by nine stars of 
which the radial velocity has been published on account of its unusually 
large amount. If our theory is correct the largest radial motions must 
be far more numerous near the vertices than at a greater distance. The 
hine stars in question are more thickly crowded (if such a word may be 
used of so small a number) within 43 degrees from the vertices than in 
the rest of the sky in the proportion of three to one. 
Taking the evidence for what itis worth, we may say that it confirms 
the theory. The proof is not convincing, however, and I will conclude by 
giving expression to my hopes that those who are in a position to test the 
whole theory by more extensive and more reliable materials will not 
neglect to do so. 
A few hundreds of stars, not pertaining to the Orion stars, and fainter 
than magnitude 3°5, must probably be sufficient for the purpose. 
