28 STATEMENTANDEXPOSITIONOr 



Long, of the asc. node of the equator ..... 110° 



Inclination of the equator . . , . . . . . 80° 



Time of rotation . . . . . . . . . 12*^1; 



motion direct. 



From these several data, it would seem probable that the equator is inclined 

 about T9i° to the plane of the planet's orbit, and some 60° to the orbits of the 

 satellites. 



So that the drawing over of material {iiiioard now, and not outward) due to the 

 proximity of the great mass of i^, would seem to have produced in the direction of 

 the plane of the equator of Uranus, an alteration like thai which, as heretofore shown, 

 (39), seems to have talcen place in the instance of another half-planet, Venus ; the 

 tilting-up (if the expression may again be tolerated) being quite as great in this 

 instance as in the other; and here the orbits of the satellites are also enormously 

 displaced. 



In the instance of Venus, it would seem that the great inclination of the equa- 

 torial plane was, (39), brought about by the attractive force of the Earth-mass of 

 greater density ; but, in the present instance, the like effect, as already shown, seems 

 to have been due to proximity of the great mass of i^; though, (3), the density 

 of the existing planet Saturn, as exhibited in Table (A), is the least in the whole 

 planetary system. 



But even that is here found to be a fact in place. For the drawing over, (41), of 

 a mass nearly equal to li^o of that of Uranus, from a region in which the mean 

 density of the nebulous material was far inferior to that of the >^-mass,^ could hardly 

 fail to have resulted in a mean density of the existing Saturn, such as we find. 



The scrupulously exact coincidence of the numbers in the column of Law with 

 those in the column of Fact in Table (B), in (14), approaches the nearest to an ex- 

 ception, in the very instance of Uranus; the existing Uranus being 0.374 of the 

 Earth's distance toithin the distance due to Uranus in accordance with Laio 2d, in 

 (10) ; though even that difference is less than J^th of the whole distance of Uranus 

 itself But this, if we give it any weight at all, is, again, a fact hi place. Uranus in 

 the drawing over of the material towards i^, may, perhaps, have somewhat fallen in. 



6. 



The acquisition of so much additional material, drawn in from a great distance, 

 must, it would seem, have the effect of giving to the condensing Saturn-mass a 

 much more oblate form than that which would otherwise have pertained to it ; 

 which seems to be confirmed by the fact that the outermost satellite is at the dis- 



' For the probable ratio of the densities here in question, see the paper of Mr. Trowbridge already 

 referred to in the Note to (3S). 



