1883.] of the Solar System . 147 
mass. Inversely as the square of distance, the force of ap- 
proaching and staying behind must decrease. 
As the central mass here moved away to 1*72 R, it had to 
remain behind with its part nearest to the sun — 
68-5 
V172 
9 
we have 1169 r — 52*4 7 = iii 6*6 r as the mean position of 
the central perihelion, as that of Jupiter; as the mass 
removed on the averted side to 2*96 R, it had to escape to — 
68*5 7+2*96 7 _ 68*5 7+2*96 7 
^2*96 1*72 
41*6 7, 
and 2006 7 + 41*6 7 = 2047*6 7, equal to the solar distance of 
Saturn. We have 52*47 and 41-6 7 as mean elongations or 
eveCtions of the two central masses; quantities with which 
the quantities 1*107 and i'io7 a = i*22 interfere as quantities 
of motion; the former as characteristic of the centre become 
perihelion, the second as that of the central aphelion, pro- 
jection of the former. 
When the body moves in remoteness i’22 slower, it moves 
in proximity $rz 2 times more rapidly ; when it moves in 
its proximity to the sun, 1*107 faster, it goes in its remoteness 
VIM07 times slower. We so have the mean into the ideal 
distances : — 
Jupiter 
1116 V ~ I Q 49 ( rounc ^ n & ro 5)* 
Saturn ... ~ 1*024 y (rounding 1*025). 
Their mutual distance is 1*72 x ro5 x 1*025 = 1*84. 
1*025 : ro 5= Vi*io7 : ^1*22. 
These disturbance figures — 
ro 25 2 = ro5 
1*05* =1*107 
I* IO7 2 = 1*22 
derived from the principal ones — 
1*72 
i*72 a = 2*96 
2*q6 2 = 8*8 
8*8 2 =77*3 
8*8 3 =680 
