Step 1: Use Kepler’s third law.
For planets revolving around the same star,
\[
T^2\propto r^3
\]
where
\[
T=\text{time period}
\]
and
\[
r=\text{orbital radius}
\]
Step 2: Write the ratio of time periods.
Given,
\[
T_A=8T_B
\]
Thus,
\[
\frac{T_A}{T_B}=8
\]
Using Kepler’s law,
\[
\left(\frac{T_A}{T_B}\right)^2
=
\left(\frac{r_A}{r_B}\right)^3
\]
\[
8^2=\left(\frac{r_A}{r_B}\right)^3
\]
\[
64=\left(\frac{r_A}{r_B}\right)^3
\]
Step 3: Find the ratio of orbital radii.
Taking cube root,
\[
\frac{r_A}{r_B}=4
\]
Thus,
\[
r_A:r_B=4:1
\]
Step 4: Use the formula for orbital velocity.
Orbital velocity is
\[
v=\sqrt{\frac{GM}{r}}
\]
Therefore,
\[
v\propto \frac{1}{\sqrt{r}}
\]
Step 5: Find the ratio of orbital velocities.
\[
\frac{v_A}{v_B}
=
\sqrt{\frac{r_B}{r_A}}
\]
\[
=
\sqrt{\frac{1}{4}}
\]
\[
=\frac{1}{2}
\]
Thus,
\[
v_A:v_B=1:2
\]
Step 6: Final conclusion.
Hence, the required ratio is
\[
\boxed{1:2}
\]