To solve the problem of finding the time period of rotation of the satellite that is 9 times closer to the Earth than the Moon, we can use Kepler's Third Law of Planetary Motion. Kepler's Third Law states:
\(\frac{T_1^2}{T_2^2} = \frac{R_1^3}{R_2^3}\)
Where:
Given that the satellite is 9 times closer to the Earth than the Moon, we have:
We are given:
Substituting the given values into Kepler’s Third Law equation:
\(\frac{T_1^2}{27^2} = \frac{\left(\frac{1}{9}R_2\right)^3}{R_2^3}\)
Simplify the equation:
\(\frac{T_1^2}{27^2} = \frac{1}{9^3}\)
\(\frac{T_1^2}{729} = \frac{1}{729}\)
Solve for \(T_1\):
\(T_1^2 = 1\)
\(T_1 = \sqrt{1}\)
Thus, \(T_1 = 1 \text{ day}\).
The correct answer is 1 day.
This calculation shows that when a satellite is 9 times closer to Earth compared to the Moon, its time period of rotation is 1 day, as per Kepler's Third Law.
Net gravitational force at the center of a square is found to be \( F_1 \) when four particles having masses \( M, 2M, 3M \) and \( 4M \) are placed at the four corners of the square as shown in figure, and it is \( F_2 \) when the positions of \( 3M \) and \( 4M \) are interchanged. The ratio \( \dfrac{F_1}{F_2} = \dfrac{\alpha}{\sqrt{5}} \). The value of \( \alpha \) is 
