CERTAIN HARMONIES OF THE SOLAR SYSTEM. 27 



1. 



The mans of the forming Saturn would be adequate to the exercise in its own 

 place of the o'ermastering attraction here supposed. 



For if from the mass of Saturn, as found in Table (A) in (3) ; viz. : — 



we subtract the mass of Si =0.00006312+, 



as computed in (41), there will remain 0.00022246 -(-, 



for the mass of the forming Saturn; before the mass due to the interior half-planet 

 g«!, had been drawn over and inward to unite with the other portion of the entire 

 mass which has gone to constitute the complete Saturn system as we now have it. 



Now as the symbol for Saturn is Vj, we" may represent this ^x?,i formative portion 

 of that planet's mass [which we just now found to be = 0.00022246 +] by the 

 symbol \. And then computing the position of the point of equai attraction, or 

 neutral point [as, heretofore, (39), in the case of Earth and Venus], we shall find 

 i^'s attraction to extend in the direction of Uranus, to the distance from the sun's 

 centre = to 16.40924, which is far beyond the distance due to the (missing) interior 

 half-planet S^ (viz., 14.64275) as found in Table (B), in (14). The attractive force 

 of the pre-existing Saturu-mass was, then, adequate in measure to the effect here 

 supposed. 



2. 



But this same limit, 16.40924, to which the attractive force of >^ extended, in 

 the direction of Uranus, this, also, is not so very far short of the limit (U),' i. e.", 

 16.91431, at which the whole planet mass would be likely to be rent to form the 

 two half-planets, Uranus and Si; it being, in that respect, a limit analogous to that 

 found to be a dividing limit in the case of Earth and Venus in which both the half- 

 planets still exist 



The very great inclination of the satellite system of Uranus to the plane of the 

 planet's orbit w:as, long ago, determined by Sir William Herschel ; the inclination 

 of the orbits of the satellites to the plane of the ecliptic being nearly 79°; and the 

 inclination to the plane of the orbit of Uranus must therefore be nearly 79°!',^ 

 while their ascending nodes on the ecliptic are nearly in longitude 166|°; motion 

 retrograde. 



And, again, the recent observations, (23), of W. Buffham, Esq., detailed in the 

 Monthly Notices of the Royal Astronomical Society, vol.xxxiii.. No. 3 (Jan. 1873), 

 lead to results at present stated by him to be " the merest approximations ;" but 

 which yet give 



' In Table (B), in (14) ^ Or 100°59' ; the motion being i-etrograde. 



