Page:Newton's Principia (1846).djvu/584

 {| style="width:100%;" cellpadding="2" align=center
 * style="width:90%" colspan=2|, its periodic time,||388
 * style="text-align:center"|“||its distance from the sun,||389
 * style="text-align:center"|“||the motion of its aphelion,||405
 * style="width:600px" colspan=2|, its quantity of matter defined,||73
 * style="text-align:center"|“||its vis insita defined,||74
 * style="text-align:center"|“||its impressed force defined,||74
 * style="text-align:center"|“||its extension, hardness, impenetrability, mobility, vis inertiæ, gravity, how discovered,||385
 * style="text-align:center"|“||subtle matter of Descartes inquired into,||320
 * style="width:600px" colspan=2| explained and demonstrated,||94
 * style="width:600px" colspan=2|, its periodic time,||388
 * style="text-align:center"|“||its distance from the sun,||389
 * style="text-align:center"|“||the motion of its aphelion,||405
 * style="width:600px" colspan=2| of first and last ratios,||95
 * style="text-align:center"|“||of transforming figures into others of the same analytical order,||141
 * style="text-align:center"|“||of fluxions,||261
 * style="text-align:center"|“||differential,||447
 * style="text-align:center"|“||of finding the quadratures of all curves very nearly true,||448
 * style="text-align:center"|“||of converging series applied to the solution of difficult problems,||nowrap="nowrap"|271, 436
 * style="width:600px" colspan=2|, the inclination of its orbit to the ecliptic greatest in the syzygies of the node with the sun, and least in the quadratures,||208
 * style="text-align:center"|“||the figure of its body collected by calculation,||454
 * style="text-align:center"|“||its librations explained,||405
 * style="text-align:center"|“||its mean apparent diameter,||453
 * style="text-align:center"|“||its true diameter,||453
 * style="text-align:center"|“||weight of bodies on its surface,||453
 * style="text-align:center"|“||its density,||453
 * style="text-align:center"|“||its quantity of matter,||453
 * style="text-align:center"|“||its mean distance from the earth, how many greatest semi-diameters of the earth contained therein,||453
 * style="text-align:center"|“||how many mean semi-diameters,||454
 * style="text-align:center"|“||its force to move the sea how great,||449
 * style="text-align:center"|“||not perceptible in experiments of pendulums, or any statical or hydrostatical observations,||452
 * style="text-align:center"|“||its periodic time,||454
 * style="text-align:center"|“||the time of its synodical revolution,||422
 * style="text-align:center"|“||its motions, and the inequalities of the same derived from their causes,||nowrap="nowrap"|413, 144
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the earth is in its perihelion; and more swiftly in the aphelion the same, its orbit being contracted,||nowrap="nowrap"|413, 444, 445
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the apogæon is in the syzygies with the sun; and more swiftly, in a contracted orbit, when the apogæon is in the quadratures,||445
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the node is in the syzygies with the sun; and more swiftly, in a contracted orbit, when the node is in the quadratures,||446
 * style="text-align:center"|“||moves slower in its quadratures with the sun, swifter in the syzygies; and by a radius drawn to the earth describes an area, in the first case less in proportion to the time, in the last case greater,||413
 * style="text-align:center"|“||the inequality of those areas computed,||420
 * style="text-align:center"|“||its orbit is more curve, and goes farther from the earth in the first case; in the last case its orbit is less curve, and comes nearer to the earth,||415
 * style="text-align:center"|“||the figure of this orbit, and the proportion of its diameters collected by computation,||423
 * style="text-align:center"|“||a method of finding the moon s distance from the earth by its horary motion,||423
 * style="text-align:center"|“||its apogæon moves more slowly when the earth is in its aphelion, more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its apogæon goes forward most swiftly when in the syzygies with the sun; and goes backward in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its eccentricity greatest when the apogæon is in the syzygies with the sun; least when the same is in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its nodes move more slowly when the earth is in its aphelion, and more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its nodes are at rest in their syzygies with the sun, and go back most swiftly in the quadratures||414
 * }
 * style="text-align:center"|“||weight of bodies on its surface,||453
 * style="text-align:center"|“||its density,||453
 * style="text-align:center"|“||its quantity of matter,||453
 * style="text-align:center"|“||its mean distance from the earth, how many greatest semi-diameters of the earth contained therein,||453
 * style="text-align:center"|“||how many mean semi-diameters,||454
 * style="text-align:center"|“||its force to move the sea how great,||449
 * style="text-align:center"|“||not perceptible in experiments of pendulums, or any statical or hydrostatical observations,||452
 * style="text-align:center"|“||its periodic time,||454
 * style="text-align:center"|“||the time of its synodical revolution,||422
 * style="text-align:center"|“||its motions, and the inequalities of the same derived from their causes,||nowrap="nowrap"|413, 144
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the earth is in its perihelion; and more swiftly in the aphelion the same, its orbit being contracted,||nowrap="nowrap"|413, 444, 445
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the apogæon is in the syzygies with the sun; and more swiftly, in a contracted orbit, when the apogæon is in the quadratures,||445
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the node is in the syzygies with the sun; and more swiftly, in a contracted orbit, when the node is in the quadratures,||446
 * style="text-align:center"|“||moves slower in its quadratures with the sun, swifter in the syzygies; and by a radius drawn to the earth describes an area, in the first case less in proportion to the time, in the last case greater,||413
 * style="text-align:center"|“||the inequality of those areas computed,||420
 * style="text-align:center"|“||its orbit is more curve, and goes farther from the earth in the first case; in the last case its orbit is less curve, and comes nearer to the earth,||415
 * style="text-align:center"|“||the figure of this orbit, and the proportion of its diameters collected by computation,||423
 * style="text-align:center"|“||a method of finding the moon s distance from the earth by its horary motion,||423
 * style="text-align:center"|“||its apogæon moves more slowly when the earth is in its aphelion, more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its apogæon goes forward most swiftly when in the syzygies with the sun; and goes backward in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its eccentricity greatest when the apogæon is in the syzygies with the sun; least when the same is in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its nodes move more slowly when the earth is in its aphelion, and more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its nodes are at rest in their syzygies with the sun, and go back most swiftly in the quadratures||414
 * }
 * style="text-align:center"|“||revolves more slowly, in a dilated orbit, when the node is in the syzygies with the sun; and more swiftly, in a contracted orbit, when the node is in the quadratures,||446
 * style="text-align:center"|“||moves slower in its quadratures with the sun, swifter in the syzygies; and by a radius drawn to the earth describes an area, in the first case less in proportion to the time, in the last case greater,||413
 * style="text-align:center"|“||the inequality of those areas computed,||420
 * style="text-align:center"|“||its orbit is more curve, and goes farther from the earth in the first case; in the last case its orbit is less curve, and comes nearer to the earth,||415
 * style="text-align:center"|“||the figure of this orbit, and the proportion of its diameters collected by computation,||423
 * style="text-align:center"|“||a method of finding the moon s distance from the earth by its horary motion,||423
 * style="text-align:center"|“||its apogæon moves more slowly when the earth is in its aphelion, more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its apogæon goes forward most swiftly when in the syzygies with the sun; and goes backward in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its eccentricity greatest when the apogæon is in the syzygies with the sun; least when the same is in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its nodes move more slowly when the earth is in its aphelion, and more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its nodes are at rest in their syzygies with the sun, and go back most swiftly in the quadratures||414
 * }
 * style="text-align:center"|“||its apogæon moves more slowly when the earth is in its aphelion, more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its apogæon goes forward most swiftly when in the syzygies with the sun; and goes backward in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its eccentricity greatest when the apogæon is in the syzygies with the sun; least when the same is in the quadratures,||nowrap="nowrap"|414, 446
 * style="text-align:center"|“||its nodes move more slowly when the earth is in its aphelion, and more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its nodes are at rest in their syzygies with the sun, and go back most swiftly in the quadratures||414
 * }
 * style="text-align:center"|“||its nodes move more slowly when the earth is in its aphelion, and more swiftly in the perihelion,||nowrap="nowrap"|414, 445
 * style="text-align:center"|“||its nodes are at rest in their syzygies with the sun, and go back most swiftly in the quadratures||414
 * }
 * }