Sect. I. Os the SOLAR SYSTEM. l§

the Sun) to S cf, the Distance from the Sunto Mars. After the fame manner the Dis-tances of Jupiter and Saturn are also found.

The mean Distance ot the Earth from theSun being made iooo, the mean Distancesof the superior Planets from the Sun are,viz. the mean Distance from the Sun of

s* J 5 2 47 . P4H

5201 >and the Excentricity< 250 >

L h 9538 J * 547 ^

To which if you add or subtract theirmean Distances, we shall have the greatestor least Distances of those Planets from theSun.

There are other Methods by which therelative Distances of the Planets might befound j but that which hath been here il-lustrated, is sufficient to evince the Certain-ty of that Problem.

Hitherto we have only considered theism theDistances of the Planets in relation to one^^f^

I another^ without determining them by any ofthePia-I known Measure; but in order to find their Theimlre(absolute Distances in some determinate Mea-"^M^.sure; there must be something given, whoseMeasure is known. Now the Circumferenceof the Earth is divided into 360 Degrees,and each of these Degrees into 60 Geogra-phical Miles, so that the whole Circum-ference contains 2 r ;6oo; and by the knownProportion for finding the Diameter of aI C 2 Circle