ch33-p031 - 31. We shall assume that the Sun is far enough...

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where R is the radius of the particle, and 2 AR π = is the cross-sectional area. On the other hand, the gravitational force on the particle is given by Newton’s law of gravitation (Eq. 13-1): 33 22 2 (4 /3) 4 3 SS S g GM m GM R GM R F rr r ρ ππ == = , where 3 mR ρπ = is the mass of the particle. When the two forces balance, the particle travels in a straight path. The condition that rg FF = implies 23 4 43 PR GM R rc r = , which can be solved to give 26 83 3 1 1 3 2 3 0 7 3 3(3.9 10 W) 16 16 (3 10 m/s)(3.5 10 kg/m )(6.67 10 m /kg s )(1.99 10 kg) 1.7 10 m . S S P R cGM πρ × ×× × × (b) Since g F varies with 3 R and r F varies with 2 , R if the radius
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This note was uploaded on 06/03/2011 for the course PHY 2049 taught by Professor Any during the Spring '08 term at University of Florida.

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