217 
Velocity of the Solar Motion. 
which the same directions are preserved, but where the extent 
of each line is made proportional to the distance of the stars 
in the second column. 
Fig. 2 is drawn according to this plan ; the angles of the 
directions remain as in the fourth column, but the lines are 
lengthened so as to give us the velocities contained in the 
sixth. 
In Fig. 4, the angles of the 3d figure are preserved, but 
the lines are again lengthened as in Fig. 2. 
N. B. These two last figures would have been of an incon- 
venient size if they had been drawn on the same scale with 
the two foregoing ones, for which reason, in comparing the 
2d and 4th with the 1st and 3d, it must be remembered that 
the former are reduced to one half of the dimensions of the 
latter. 
Remarks on the sidereal Motions as they are represented from 
Observation. 
As we have now before us a set of figures which give a 
complete view of the result of the calculations contained in 
the Xth Table, we may examine the arrangements of the stars, 
and draw a few conclusions from them, that will throw some 
light upon the subject of our present inquiry. 
In the first place, then, we have to observe in Fig. 1, that 
27 out of the 21 stars, whose motions are directed towards 
the north, are crowded together into a compass of little more 
than 76^ degrees. But this figure, as we have shown, is 
drawn from observation. We are consequently obliged to 
conclude, that, if these motions are the real ones, there must 
be some physical cause which gives a bias to the directions in 
Mocccvr, F f 
