Wherefore, Out of your Sector, (it being ftill opened to the former distance) take the diftance of the Aphelial Point of the Earth (for MARS 611) and fet it (upon the Earths Apheliat Line) from the Centre o to 4p., fo fhall the point Ap. be the Aphelial Point of the Earth And the diftance of the Excentric of the Earth, from the Aphelial Point of the Earth being 600,take 600 out of the Sector, and fet it from the Earths Aphelial Point Ap. downwards towards the Centre O, and that fhall be the Centre whereon to defcribe the Orbit of the Earth on the Theory of MARS. Which Point falling fo near the Centre O, you may defcribe the Earths Orbit upon the Centre it felf the difference being only Parts: And in the Theories of the other two Superior Planets, the difference wil be much lefs; for in the Theory of Saturn it will be Parts: And in the Theory of Jupiter, but Parts: So that in fmall Theories they need not be much regarded. Το T 4. For the Aphelial and Excentric Points of the Earth, and the two Inferior Planets and, the Tables following will ex-hibit. Fig. LXXVI. 5. For the Nodes of the Planets. The Afcendant Nodes of the feveral Planets (for the Earth hath none :) This Table will tell you to what Points in the Ecliptic they are to be drawn. For d. Wherefore, the Node of the Planet & being in 17.55 de. of 8, lay a Ruler from the Centre to 17.55 de. of Taurus, and there draw an obfcure Line: This Line is the common Section of plain Planets Excentric, with the Plain of the Ecliptic; and where this Line croffeth the Orbit of Mars, there write Dragons Head; at which Point, when any Planet is in its Orbit, it goes into North Latitude: And at the oppofite Point, through the Centre, is the place of the Dragons Tail, where it goes into South Latitude. "Of the Inclination of the Planets. The Greatest Inclination of the Planets are fuch as are expreffed in this Table. The Aphelian Lines and Orbits of the Earth, and any of the Planets being drawn within the Ecliptick Circle, the next thing to be done is, to fhew how to place the Earth and any Planet in their refpective Orbits, for any Time propofed And alfo, How to Reduce their Places fo found in their Orbits at that time, to their refpective Places in the Ecliptick Circle. In order whereunto it will be neceflary to fhew, I. How Time is to be Accounted. II. To Collect the Anomalies of the Earth and Planet for Time propofed. any Fig. LXXVI.. III. How Degrees of Anomaly in the Orbits, are to be reduced to TIM CHA P. II. A How Time is to be Accounted. IME is to be thus Accounted: Any Day begins upon its own Noon So that 12 at Noon of the first Day of January, is the Common Term of the Old and New Tears; it being the End of the Former, and the Beginning of the Latter. Before the Longitude or Place of a Planet in the Ecliptic can be found; the equal Motion of the Anomaly for the Time propofed must be known; and that Motion for any propofed Time may be collected out of thefe TABLES.. 354 100 ૐ 100 Years.De. Pts. De. Pts. De, Pts. De. Pts. De. Pts. De. Pts. 1692 194 34 346. 17 246. 08 126. 89 247. 04 167. 86 1700 194. 26 83.88 08 194 181181. 59 128. 88 218. 08 248. 42 245. 58 254. 48 40. 45 251. 17 41. 01 17. 01 137. 28 131. 63 252. $118. 73 32 193. 95 114. 72 20. 08 222. 81 253. 93 196. 45 40 193. 87 212. 43 252. 88 314. 00 255. 31 274. 17 48 193. 80 310. 14 145. 68 45. 18 256. 68 351. 89 56 193. 72 47. 86 28. 48 136. 40 258. 06 69. 61 72 193. 57 243. 28 154. 08 318. 76 260. 81 225. 05 80 193. 49 341. 08 36. 88 49. 94 262. 19 302. 77 96 193. 34 78. 71 162. 48 232. 30 264. 94 98. 21 1800 193. 30 225. 27 283. 88 277. 90 85. 63 317 35 Motion of the Anomaly, in Months Of the Common YEAR. May July Pts. De. Pts.De. Pts. April 118. 27 4. CI 9. 97 April May Fune 16. 24 49. 67 126. 86 Fanua. 30. 55 1.04; 2. 58, |