Step 1: Applying Kepler’s Third Law.
For satellites orbiting the same central body:
\[
T^2 \propto r^3
\]
This gives:
\[
\frac{T_2}{T_1} = \left(\frac{r_2}{r_1}\right)^{3/2}
\]
Step 2: Substituting given values.
Given:
\[
T_1 = 2 \, \text{years}, \quad r_2 = 2R, \quad r_1 = R
\]
So:
\[
\frac{T_2}{2} = (2)^{3/2}
\]
Step 3: Evaluating power term.
\[
(2)^{3/2} = \sqrt{2^3} = \sqrt{8} = 2.828
\]
Step 4: Calculating time period of satellite Q.
\[
T_2 = 2 \times 2.828 = 5.656
\]
Step 5: Approximation.
\[
T_2 \approx 5.6 \, \text{years}
\]
Step 6: Final conclusion.
\[
\boxed{5.6 \, \text{years}}
\]