Let's first find the distance of the satellite from the center of the Earth from the Kepler's Third Law:
T 2 R 3 = 4 π 2 G M E , \frac{T^2}{R^3} = \frac{4\pi^2}{GM_E}, R 3 T 2 = G M E 4 π 2 , here,
T T T is the period that the satellite needs to make one revolution,
R R R is the distance of the satellite from the center of the Earth,
G G G is the universal gravitational constant and
M E M_E M E is the mass of the Earth.
Then, from this equation we can find the distance
of the satellite from the center of the Earth:
R = G M T 2 4 π 2 3 . R = \sqrt[3]{\frac{GMT^2}{4\pi^2}}. R = 3 4 π 2 GM T 2 . Let's substitute the numbers:
R = 6.67 ⋅ 1 0 − 11 N m 2 k g 2 ⋅ 5.98 ⋅ 1 0 24 k g ⋅ ( 6.0 h r ⋅ 3600 s 1 h r ) 2 4 π 2 3 = 1.67 ⋅ 1 0 7 m . R = \sqrt[3]{\frac{6.67 \cdot 10^{-11} \frac{Nm^2}{kg^2} \cdot 5.98 \cdot 10^{24} kg \cdot (6.0 hr \cdot \frac{3600 s}{1 hr})^2}{4\pi^2}} = 1.67 \cdot 10^7 m. R = 3 4 π 2 6.67 ⋅ 1 0 − 11 k g 2 N m 2 ⋅ 5.98 ⋅ 1 0 24 k g ⋅ ( 6.0 h r ⋅ 1 h r 3600 s ) 2 = 1.67 ⋅ 1 0 7 m . We can find the height of the satellite above the Earth's surface from the formula:
R = R E a r t h + h , R = R_{Earth} + h, R = R E a r t h + h , here,
R E a r t h R_{Earth} R E a r t h is the radius of the Earth,
h h h is the height of the satellite above the Earth's surface.
Finally, we get:
h = R − R E a r t h = 1.67 ⋅ 1 0 7 m − 6.37 ⋅ 1 0 6 m = 1.03 ⋅ 1 0 7 m . h = R - R_{Earth} = 1.67 \cdot 10^7 m - 6.37 \cdot 10^6 m = 1.03 \cdot 10^7 m. h = R − R E a r t h = 1.67 ⋅ 1 0 7 m − 6.37 ⋅ 1 0 6 m = 1.03 ⋅ 1 0 7 m . Answer:
h = 1.03 ⋅ 1 0 7 m h = 1.03 \cdot 10^7 m h = 1.03 ⋅ 1 0 7 m .
Comments
Thanks. Correct answer