Step 1:
Kepler’s third law states:
\[
T^2 = \frac{4\pi^2 r^3}{GM}
\]
where:
- \( T \) is the orbital period of the planet,
- \( r \) is the mean distance from the sun,
- \( G \) is the gravitational constant,
- \( M \) is the mass of the sun.
Step 2:
The slope of the graph between \( T^2 \) and \( r^3 \) will be:
\[
{slope} = \frac{4\pi^2}{GM}
\]
Step 3:
This is the required slope, and it depends on the mass of the sun and the gravitational constant.