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1 here fuppose the Linea Apsidum fixt, as having na Argument from Ob-lervation to prove the contrary, though it be very probable that as the Apo-pam of our Moon has a Motion about the Eartb in about 9 Years, so that dfthi$ Satellite oyght to have about Satum, byt witlj a much Lopger Period,whieh future Ob(ervation may discovef.

The distance of thjs Satellite from the Center os Saturn feems to be muchabout 4 Diameters of the Rjng, or 9 of the Globe, and the Plane wherein itmoves very little or nothing aifiering from that of the Rjng, that is to fcyintersecting the Orb of Satum 4* n° and io s zx° a i a T, with at) An-gle of Degrecs, lo as tobe nearly Parallel to the Eartljs liquator, whcncethe batitude of the Apogxon Semicircle from 4* to Ic s ai° of Satum s Lon-gitudo from the First: Star of T, will be Northern, and of the other SemiciftleSouthern; and the contrary in the other half of Saturns Longitudo, to wit,from ic 5 ix° to 4 S of his distance from the First Star of T.

It follows now to stiew how by the help of tljis Table to computc theplace of this Satellite, to any time required.

First wc muli haye the true Longitudo of Satum from the Eartb, andnumbred from the First Star of T, ( or rather the Place of the Earth yiew-.ed from Satum together with its Latitude from the Orb of Satum, bin thatbcing never fully i of a degree we neglect it as a Nicety) and therefromsubstract ics there remains the distance of Satum from this EquinoctialPoint, with whieh djstance as with the Longitudo of the Sun, take out theRjgbt Asicenfion and Declination thereto (i 3} degrees bcing thfi Oh liquit ycommon to both) and to the Rjght Asicenfion adding iq s the Summ {halfbe the Longitudo of the Satellit’ s Apogxon. Then läy, as Radius to Sine ofthe Declination, so 8 to the greatest Latitude in Apogao, or Pcrigfio in theparts of the Semidiameter of the Rjng.

Next Collect the Middle Motion of the Satellite, and f oflj. it Substractic s zz° the remainder shall be the mean Anomaly, with whieh in the Tableof the Moon s Primary Equation, take out the Equation anlwerjng thereto,and the half thereof added or sobstracted to or frosn the Middle Mption, 9^cording to the Table, gives the True Motion of the Satellite, from whiehsttbstract the Apog.eon, and if the remainder be more thari 6 Signi* theSatellite is Occidental, if leis Oriental j and as Rjidius to Sine of the remainsder, io 8 to the Semidiameters of the Rjng, or 18 to the Semidiajneters ofthe Globe, that the Satellite is to the Eastward or Wqstward of the Ccute<of Satum, according to the aforegoing Precept.

Lastly, as Rajiut to Co-sine of the said Remainder, so is the greatest La-titude from the Eine of the Ansa, to the Latitude sought.

Here Note, that I purposely neglect the Inequality of the distance arisingfrom the Ecccntricitj, as being' toq sinall to be any Way obsorvable.

Lastly to ciear all diificulties that may arifc to them that are but little!veried in this fort of Calculation, I have added an Example of the!Work, that wfiere the precept may seem obscure it may be thereby illu-!stmted. :

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