221 
and Velocity of the Solar Motion . 
The remark that stars having a side motion, are not affected 
by the cause of the compression or expansion, which acts 
upon the rest, is perfectly explained ; for a parallactic motion, 
in the direction of the motion of Arcturus, can have no effect 
in lengthening or shortening the perpendicular distance to 
which a star may move in a side direction. 
I have only to add, that the small velocities of Rigel, 
u Orionis, Spica, and Antares, in Fig. 4, as well as the great 
velocities of Arcturus, Procyon, and Sirius, point out the same 
apex which in the first part of this Paper has already been 
established by more extended computations. 
The case of Aldebaran, though seemingly contrary to what 
has been shown, confirms the same conclusions. This will 
appear by considering that a star, moving towards the solar 
apex with a greater real motion than its parallactic one, must 
continue apparently to move in its real direction ; but should 
a star, such as Aldebaran, move towards the apex with less 
velocity than the parallactic motion which opposes it, there 
will arise a change of direction, and the star will be seen 
moving towards the opposite part of the heavens. 
Trial of the Method to obtain the Quantity of the Solar Motion 
by its Rank among the sidereal Velocities . 
According to the conditions that have been explained, a 
calculation may be made with a view of equalizing the velo- 
cities of the sun and the star a. Orionis ; and the result of it 
will show that the proposed equality will be obtained when 
the solar motion is 1", 266230. It will moreover be found 
than so small an increase of this motion as o",oi would give 
us 19 stars with less, and 17 with more velocity than that 
