Chapter 13393Section 13.7Energy Considerations in Planetary and Satellite MotionP13.331211 1222mvGM mrrmviEfif+−FHGIKJ=120112vGMRvEfFHGIKJ=orvvGMRfEE2122=−andGMRfEEFHGIKJ12122vf=×−×LNMOQP=×2 00 101 25 101 66 104284...ejmsP13.34(a)vMGREsolar escapeSunSunkm s==⋅242 1.(b)Let rRxES=⋅represent variable distance from the Sun, with xin astronomical units.vRxx⋅242 1Sun.If v=125 000 km3 600 s, then x×1 472 20 1011A.U.m(at or beyond the orbit of Mars, 125 000 km/h is sufficient for escape).P13.35To obtain the orbital velocity, we useFmMGRmvR∑22orvMGR=We can obtain the escape velocity from12mvmMGResc2=orvMGRvesc22P13.36vRhGMiEEE22+=+bgKmvGM miiEE+FHGIKJ=×⋅××+×LNMMOQPP−1212126 67 105 98 10500637 100500 10145 10211246610.N mkgkgkgm mJejejThe 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 .