Answer
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Hint: Kepler's laws of motion for planets are three scientific laws describing the motion of planets around the Sun. Kepler’s third law has improved the model of Copernicus.
Formula used: Kepler’s third law: \[T\propto {{r}^{\dfrac{3}{2}}}\] where, T = the time period and r = distance and, satellitic kinetic energy \[K=\dfrac{GMm}{2r}\], where M = mass of earth, m= mass of satellite, G = gravitational constant.
Complete step by step solution:
We have to use Kepler’s third law which is given by,
\[\begin{align}
& T\propto {{r}^{\dfrac{3}{2}}} \\
& \Rightarrow r\propto {{T}^{\dfrac{2}{3}}}............(i) \\
\end{align}\]
Now, from kinetic energy formula we get,
\[K=\dfrac{GMm}{2r}\] which means \[K\propto \dfrac{1}{r}...................(ii)\]
Substituting, equation (i) in (ii) we get,
\[K\propto \dfrac{1}{{{T}^{\dfrac{2}{3}}}}\propto {{T}^{-\dfrac{2}{3}}}\]
So, the answer is option D.
Note: Kepler's laws of motion for planets is the concept dealing with the distance of planets from the sun and their orbital periods.
Formula used: Kepler’s third law: \[T\propto {{r}^{\dfrac{3}{2}}}\] where, T = the time period and r = distance and, satellitic kinetic energy \[K=\dfrac{GMm}{2r}\], where M = mass of earth, m= mass of satellite, G = gravitational constant.
Complete step by step solution:
We have to use Kepler’s third law which is given by,
\[\begin{align}
& T\propto {{r}^{\dfrac{3}{2}}} \\
& \Rightarrow r\propto {{T}^{\dfrac{2}{3}}}............(i) \\
\end{align}\]
Now, from kinetic energy formula we get,
\[K=\dfrac{GMm}{2r}\] which means \[K\propto \dfrac{1}{r}...................(ii)\]
Substituting, equation (i) in (ii) we get,
\[K\propto \dfrac{1}{{{T}^{\dfrac{2}{3}}}}\propto {{T}^{-\dfrac{2}{3}}}\]
So, the answer is option D.
Note: Kepler's laws of motion for planets is the concept dealing with the distance of planets from the sun and their orbital periods.
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