On the Connexion of the Physical SciencesJ. Murray, 1858 - 523 pages |
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Page 15
... equal spaces or areas in equal times ; a circumstance which is independent of the law of the force , and would be the same whether it varied inversely as the square of the distance , or not , provided only that it be directed to the ...
... equal spaces or areas in equal times ; a circumstance which is independent of the law of the force , and would be the same whether it varied inversely as the square of the distance , or not , provided only that it be directed to the ...
Page 25
... equal to twice that of Jupiter ; a relation which the sagacity of La Place perceived to be the cause of a periodic irregularity in the mean motion of each of these planets , which completes its period in nearly 918 years , the one being ...
... equal to twice that of Jupiter ; a relation which the sagacity of La Place perceived to be the cause of a periodic irregularity in the mean motion of each of these planets , which completes its period in nearly 918 years , the one being ...
Page 28
... equal on both sides of it . But , as their orbits have a small inclination to the plane of the planet's equator , there is a want of symmetry , and the action of the protuberant matter tends to make the nodes regress by pulling the ...
... equal on both sides of it . But , as their orbits have a small inclination to the plane of the planet's equator , there is a want of symmetry , and the action of the protuberant matter tends to make the nodes regress by pulling the ...
Page 29
... equal to three times that of the second ; and that the mean longitude of the first satellite , minus three times that of the second , plus twice that of the third , is always equal to two right angles . It is proved by theory , that ...
... equal to three times that of the second ; and that the mean longitude of the first satellite , minus three times that of the second , plus twice that of the third , is always equal to two right angles . It is proved by theory , that ...
Page 40
... equal to the apparent diameter of the sun , as seen from the centre of the moon . The mean duration of a revolution of the sun , with regard to the node of the lunar orbit , is to the duration of a synodic revolution ( N. 113 ) of the ...
... equal to the apparent diameter of the sun , as seen from the centre of the moon . The mean duration of a revolution of the sun , with regard to the node of the lunar orbit , is to the duration of a synodic revolution ( N. 113 ) of the ...
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61 Cygni absorbed action appears atmosphere attraction bismuth blue bodies centre centrifugal force chemical circular polarization coloured rings comet consequently copper crystal dark density diamagnetic diameter diminishes direction distance disturbing earth ecliptic effect electricity equal equator ethereal medium excentricity experiments extreme force gravitation greater heat hemisphere increase intensity Jupiter latitude length lines liquid longitude luminous lunar magnetic mass mean meridian metallic miles molecules moon motion move nebula nodal lines nodes NOTE nutation observed optic axis orbit parallax paramagnetic particles passing perihelion period perpendicular phenomena plane polarized light pole position prism produced quantity rays reflected refraction refrangible retrograde motion revolution revolving right angles rotation round satellites Sir John Herschel solar spectrum sound space stars substances sun's surface telescope temperature terrestrial theory tion tourmaline transmitted tricity undulations Uranus vapour velocity vibrations violet visible Voltaic waves wire