391_Physics ProblemsTechnical Physics

391_Physics ProblemsTechnical Physics - Chapter 13 Section...

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Chapter 13 393 Section 13.7 Energy Considerations in Planetary and Satellite Motion P13.33 1 2 11 1 2 22 mv GM m rr mv iE fi f +− F H G I K J = 1 2 0 11 2 vG M R v E f F H G I K J = or vv GM R f E E 2 1 2 2 =− and GM R f E E F H G I K J 1 2 12 2 v f =×− × L N M O Q P 2 00 10 1 25 10 1 66 10 4 2 8 4 .. . ej ms P13.34 (a) v MG R E solar escape Sun Sun km s == 2 42 1 . (b) Let rRx ES = represent variable distance from the Sun, with x in astronomical units. v Rx x 2 42 1 Sun . If v = 125 000 km 3 600 s , then x × 1 47 2 20 10 11 A.U. m (at or beyond the orbit of Mars, 125 000 km/h is sufficient for escape). P13.35 To obtain the orbital velocity, we use F mMG R mv R 2 2 or v MG R = We can obtain the escape velocity from 1 2 mv mMG R esc 2 = or v MG R v esc 2 2 P13.36 v Rh GM i E E E 2 2 + = + bg Km v GM m ii E E + F H G I K J = ×⋅ × ×+ × L N M M O Q P P 1 2 1 2 1 2 6 67 10 5 98 10 500 637 10 0500 10 145 10 2 11 24 66 10 . N m kg kg kg m m J e j e j The change in gravitational potential energy of the satellite-Earth system is
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This note was uploaded on 12/14/2011 for the course PHY 203 taught by Professor Staff during the Fall '11 term at Indiana State University .

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