At great distances from the planet, if neglecting other gravitational influences, the rock will reach a speed close to 
Explanation:
To express the velocity that is very far from the planet alongside the escape velocity, we utilize the principles of energy conservation, allowing us to derive
The initial velocity of the rock,
. Given that the radius is R, we can determine the escape velocity using the following formula:




Where M represents the mass of the planet and G represents the gravitational constant.
Based on the given conditions,
Surface potential energy can be articulated as, 
As R approaches infinity when distanced from the planet, thus 
Then, the initialkinetic energy will be expressed as

Simultaneously, the finalkinetic energy can be described as
Here,
Now, adding the potential and kinetic energies at the beginning and end gives the equation to determine the final velocity
expressed as
By canceling 'm' common on both sides, we yield

Recognizing that
, we can rewrite it as
, we arrive at


Taking the squares out leads to
