day04keplerlaws

day04keplerlaws - K s && = R 3 T 2 = Gm s...

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Kepler’s Laws 1. The planets move about the sun in elliptical orbits, with the sun at one focus. 2. The straight line joining the sun and a given planet sweeps out equal areas in equal intervals of time. 3. The square of the period of revolution of a planet about the sun is proportional to the cube of its mean distance from the sun. For the Earth: (Derivation) F c = F g m s ( 4 ± 2 R T 2 )= Gm E m s R 2 (for circular orbits) (* s = satellite) K E = R 3 T 2 = Gm E 4 ± 2 = 1.01 x 10 13 m 3 / s 2 For sun satellites ( e.g. planets, asteroids, etc.)
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Unformatted text preview: K s && = R 3 T 2 = Gm s && 4 2 = 3.35 x 10 18 m 3 / s 2 (** s = sun) A:\sph4u1\chap6\day04keplerlaws.doc NOTES: using R 3 T 2 for each of the planets yields slightly different K s s due to experimental errors. a) R is the centre to centre distance (e.g. radius of planets orbit) b) T refers to the period of the orbiting object (e.g. the planet) c) m, in the Law is that of the object being orbited. (e.g. the sun)...
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This note was uploaded on 10/27/2011 for the course PHYSICS 1028 taught by Professor C.jones during the Spring '09 term at UWO.

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day04keplerlaws - K s && = R 3 T 2 = Gm s...

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