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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.
- Spring '09