Step 1: Use Kepler’s Third Law.
According to Kepler’s Third Law of planetary motion:
\[
T^2 \propto r^3
\]
where \(T\) is time period and \(r\) is distance from the Sun.
Step 2: Write proportional relation.
\[
\frac{T_2^2}{T_1^2} = \frac{r_2^3}{r_1^3}
\]
Step 3: Substitute given condition.
If distance is doubled:
\[
r_2 = 2r_1
\]
So,
\[
\frac{T_2^2}{T^2} = \frac{(2r)^3}{r^3}
\]
\[
\frac{T_2^2}{T^2} = 8
\]
Step 4: Take square root.
\[
\frac{T_2}{T} = \sqrt{8}
\]
\[
\frac{T_2}{T} = 2\sqrt{2}
\]
Step 5: Final result.
\[
T_2 = 2\sqrt{2}\,T
\]
\[
\boxed{2\sqrt{2}\,T}
\]