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Unformatted text preview: constants and the mass of the Sun. Therefore we can write a similar equation for any planet that orbits the Sun. T 1 2 /r 1 3 = 4 2 /G . M S EQ.5 T 2 2 /r 2 3 = 4 2 /G . M S EQ.6 And therefore can write Keplers third law T 1 2 /r 1 3 = T 2 2 /r 2 3 EQ.7 This was a magnificent result for Newtons theory. Incidentally, scientists could then use these results to find the mass of the sun for the first time. Writing EQ.5 for the Earth-Sun system, we have T E 2 /r ES 3 = 4 2 /G . M S EQ.8 where T E = 3.16x10 7 sec r ES = 1.50x10 11 m G = 6.67x10-11 N m 2 /kg 2 Solving for the mass of the Sun we have M S = [4 2 /G] r ES 3 /T E 2 EQ.9 M S = 2.0x10 30 kg...
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- Spring '09