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Unformatted text preview: . However we do know that the speed v of a satellite is
equal to the circumference (2π r) of its orbit divided by the period T, so v = 2 π r / T . Chapter 5 Problems 263 SOLUTION Solving the relation v = 2 π r / T for r gives r = vT / 2π . Substituting this value
for r into Equation (1) yields
3/2
v T / ( 2π ) TA
rA = 3/2 = A A
=
3/ 2
TB
rB
vB TB / ( 2π ) 3/ 2 ( vA TA )
3/ 2
( vB TB ) 3/ 2 Squaring both sides of this equation, algebraically solving for the ratio TA/TB, and using the
fact that vA = 3vB gives
3
3
TA
vB
vB
1
= 3=
=
3
TB
vA
( 3vB ) 27 ______________________________________________________________________________
36. REASONING AND SOLUTION The period of the moon's motion (approximately the
length of a month) is given by
T= 4π 2 r 3
=
GM E 4π 2 ( 3.85 × 108 m )
( 6.67 ×10−11 N ⋅ m 2 / kg 2 )( 5.98 ×1024 kg )
3 = 2.38 × 106 s = 27.5 days 37. SSM REASONING Equation 5.2 for the centripetal acceleration applies to both the plane
and the satellite, and the centripetal acceleration is the same for each. Thus, we have ac = 2
v plane rplane = 2
v satellite rsatellite or v plane = Fr
Gr
G
H plane satellite I
v
J
J
K satellite The speed of the satellite can be obtained directly from Equation 5.5.
SOLUTION Using Equation 5.5, we can express the speed of the satellite as
v satellite = Gm E
rsatellite Substituting this expression into the expression obtained in the reasoning for the speed of the
plane gives 264 DYNAMICS OF UNIFORM CIRCULAR MOTION Fr I
Fr
v
=G
Gr J
GJ
H K Gr
H
15 c
b mg6.67 × 10 N ⋅ m
= v plane = plane plane satellite satellite satellite −11 v plane 2 I Gm r
Jr = r
J
K
/ kg h
5.98
c × 10 plane E satellite GmE satellite 2 24 6.7 × 10 6 m kg h
= 12 m / s GM S
r
− 11
2
2
(Equation 5.5), where MS is the mass of the star, G = 6.674 × 10
N ⋅ m / kg is the
universal gravitational constant, and r is the orbital radius. This expression can be solved for
2π r
MS. However, the orbital radius r is not known, so we will use the relation v =
T
(Equation 5.1) to eliminate r in favor of the known quantities v and T (the period). Returning
to Equation 5.5, we square both sides and solve for the mass of the star: 38. REASONING The speed v of a planet orbiting a star is given by v = GM S
= v2
r Then, solving v = or MS = rv 2
G (1) 2π r
vT
for r yields r =
, which we substitute into Equation (1):
T
2π vT 2 v
3
rv 2π = v T
MS =
=
G
G
2π G
2 (2) We will use Equation (2) to calculate the mass of the star in part a. In part b, we will solve
Equation (2) for the period T of the faster planet, which should be shorter than that of the
slower planet. SOLUTION
a. The speed of the slower planet is v = 43.3 km/s = 43.3×103 m/s. Its orbital period in
seconds is T = (7.60 yr)[(3.156 × 107 s)/(1 yr)] = 2.40×108 s. Substituting these values into
Equation (2) yields the mass of the star: ( )(
3 )
) 43.3 × 103 m/s 2.40 × 108 s
v 3T
MS =
=
= 4.65 × 1031 kg
−11
2
2
2π G 2π 6.674 × 10
N ⋅ m / kg ( This is roughly 23 times the mass of the sun. Chapter 5 Problems 265 b. Solving Equation (2) for the orbital period T, we obtain
v 3T
= MS
2π G or T= 2π GM S (3) v3 The speed of the faster planet is v = 58.6 km/s = 58.6 × 103 m/s. Equation (3) now gives the
orbital period of the faster planet in seconds: T= ( )(
3
(58.6 ×103 m/s ) 2π 6.674 ×10−11 N ⋅ m2 / kg 2 4.65 ×1031 kg ) = 9.69 ×107 s Lastly, we convert the period from seconds to years: ( ) 1 yr
T = 9.69 ×107 s 7 3.156 ×10 s = 3.07 yr 39. REASONING The satellite’s true weight W when at rest on the surface of the planet is the
gravitational force the planet exerts on it. This force is given by W = GM P m r 2
(Equation 4.4), where G is the universal gravitational constant, MP is the mass of the planet,
m is the mass of the satellite, and r is the distance between the satellite and the center of the
planet. When the satellite is at rest on the planet’s surface, its distance from the planet’s
2
center is RP, the radius of the planet, so we have W = GM P m RP . The satellite’s mass m is
given, as is the planet’s radius RP. But we must use the relation T = 2π r 3 2
(Equation 5.6)
GM P to determine the planet’s mass MP in terms of the satellite’s orbital period T and orbital
radius r. Squaring both sides of Equation 5.6 and solving for MP, we obtain T2 = ()
2
( GM P ) 22 π 2 r 3 2 Substituting Equation (1) into W = W= 2 = 4π 2 r 3
GM P GM P m
2
RP or MP = 4π 2 r 3
GT 2 (1) (Equation 4.4), we find that Gm
G m 4π 2 r 3 4π 2r 3m
MP ) = 2 = 2 2
2( RP
RP G T 2 RPT (2) 266 DYNAMICS OF UNIFORM CIRCULAR MOTION SOLUTION All of the quantities in Equation (2), except for the period T, are given in SI
base units, so we must convert the period from hours to seconds, the SI base unit for time:
T = (2.00 h)[(3600 s)/(1 h)] = 7.20×103 s. The satellite’s orbital radius r in Equation (2) is
the distance between the satellite and the center of the orbit, which is the planet’s center.
Therefore, the orbital radius is the sum of the planet’s radius RP and the satellite’s height h...
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This note was uploaded on 04/30/2013 for the course PHYS 1100 and 2 taught by Professor Chastain during the Spring '13 term at LSU.
 Spring '13
 CHASTAIN
 Physics, The Lottery

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