Step 1: Formula for escape velocity.
The escape velocity \( v_e \) from a planet is given by:
\[
v_e = \sqrt{\frac{2GM}{R}}
\]
where \( G \) is the gravitational constant, \( M \) is the mass of the planet, and \( R \) is the radius of the planet.
Step 2: Relating escape velocities and radii.
We are given that the ratio of escape velocities from planets A and B is \( 3:2 \), and the ratio of their radii is \( 2:3 \). Let \( v_{eA} \) and \( v_{eB} \) be the escape velocities, and \( R_A \) and \( R_B \) be the radii of planets A and B, respectively. We know:
\[
\frac{v_{eA}}{v_{eB}} = \frac{3}{2}, \quad \frac{R_A}{R_B} = \frac{2}{3}
\]
Step 3: Express escape velocity in terms of acceleration due to gravity.
The escape velocity is related to the acceleration due to gravity \( g \) at the surface of a planet by the formula:
\[
v_e = \sqrt{2gR}
\]
Therefore, for planets A and B:
\[
v_{eA} = \sqrt{2g_A R_A}, \quad v_{eB} = \sqrt{2g_B R_B}
\]
Squaring both equations:
\[
v_{eA}^2 = 2g_A R_A, \quad v_{eB}^2 = 2g_B R_B
\]
Taking the ratio of the escape velocities squared:
\[
\frac{v_{eA}^2}{v_{eB}^2} = \frac{g_A R_A}{g_B R_B}
\]
Using the given ratios:
\[
\left( \frac{3}{2} \right)^2 = \frac{g_A R_A}{g_B R_B}
\]
Simplifying:
\[
\frac{9}{4} = \frac{g_A R_A}{g_B R_B}
\]
Substitute \( \frac{R_A}{R_B} = \frac{2}{3} \):
\[
\frac{9}{4} = \frac{g_A \cdot \frac{2}{3}}{g_B}
\]
Solving for \( \frac{g_A}{g_B} \):
\[
\frac{g_A}{g_B} = \frac{9}{4} \cdot \frac{3}{2} = \frac{27}{8}
\]
Step 4: Final ratio.
Thus, the ratio of the acceleration due to gravity at the surface of A to that at the surface of B is:
\[
\frac{g_A}{g_B} = \frac{27}{8}
\]