16h.10′. The places of this comet computed in this orbit by Mr. Bradley, and compared with the places observed by himself, his uncle Mr. Pound, and Dr. Halley, may be seen in the following table.
| 1723 Eq. Time. |
Comet's Long. obs. |
Lat. Nor. obs. |
Comet's Lon. com. |
Lat.Nor. comp. |
Diff. Lon. |
Diff. Lat. |
| d. h. ′ Oct. 9.8. 5 10.6.21 12.7.22 14.8.57 15.6.35 21.6.22 22. 6.24 24.8. 2 29.8.56 30.6.20 Nov. 5.5.53 8.7. 6 14.6.20 20.7.45 Dec. 7.6.45 |
° ′ ″ ♒ 7.22.15 6.41.12 5.39.58 4.59.49 4.47.41 4. 2.32 3.59. 2 3.55.29 3.56.17 3.58. 9 4.16.30 4.29.36 5. 2.16 5.42.20 8. 4.13 |
° ′ ″ 5. 2. 0 7.44.13 11.55. 0 14.43.50 15.40.51 19.41.49 20. 8.12 20.55.18 22.20.27 22.32.28 23.38 33 24. 4.30 24.48.46 25.24.45 26.54.18 |
° ′ ″ ♒ 7.21.26 6.41.42 5.40.19 5. 0.37 4.47.45 4. 2.21 3.59.10 3.55.11 3.56.42 3.58.17 4.16.23 4.29.54 5. 2.51 5.43.13 8. 3.55 |
° ′ ″ 5. 2 47 7.43.18 11.54.55 14.44. 1 15.40.55 19.42. 3 20. 8.17 20.55. 9 22.20.10 22.32.12 23.38. 7 24. 4.40 24.48.16 25.25.17 26.53.42 |
″ + 49 - 50 - 21 - 48 - 4 + 11 - 8 + 18 - 25 - 8 + 7 - 18 - 35 - 53 + 18 |
″ - 47 + 55 + 5 - 11 - 4 - 14 - 5 + 9 + 17 + 16 + 26 - 10 + 30 - 32 + 36 |
From these examples it is abundantly evident that the motions of comets are no less accurately represented by our theory than the motions of the planets commonly are by the theories of them; and, therefore, by means of this theory, we may enumerate the orbits of comets, and so discover the periodic time of a comet's revolution in any orbit; whence, at last, we shall have the transverse diameters of their elliptic orbits and their aphelion distances.
That retrograde comet which appeared in the year 1607 described an orbit whose ascending node (according to Dr. Halley's computation) was in ♉ 20° 21′; and the inclination of the plane of the orbit to the plane of the ecliptic 17° 2′; whose perihelion was in ♒ 2° 16′; and its perihelion distance from the sun 58680 of such parts as the radius of the orbis magnus contains 100000; and the comet was in its perihelion October 16d.3h.50′; which orbit agrees very nearly with the orbit of the comet which was seen in 1682. If these were not two different comets, but one and the same, that comet will finish one revolution in the space of 75 years; and the greater axis of its orbit will be to the greater axis of the orbis magnus as to 1, or as 1778 to 100, nearly. And the aphelion distance of this comet from the sun will be to the mean distance of the earth from the sun as about 35 to 1; from which data it will be no hard matter to determine the elliptic orbit of this comet. But these things are to be supposed on condition, that, after the space of 75 years, the same comet shall return again in the same orbit. The other comets seem to ascend to greater heights, and to require a longer time to perform their revolutions.
But, because of the great number of comets, of the great distance of their
