If I reach escape velocity, does that mean I stop being pulled by the planet's gravity?

No. Gravity extends infinitely, so you are always pulled. Escape velocity is the speed where your kinetic energy is exactly equal to the negative gravitational potential energy. This means you have just enough speed to coast infinitely far away, slowing down continuously but never falling back. At any finite distance, gravity is still acting on you, just very weakly.

Why is the escape velocity for Earth about 11.2 km/s, but rockets don't need to reach that speed all at once?

The escape velocity formula assumes a single impulsive burst from the surface with no further thrust. Real rockets provide continuous thrust over minutes, fighting gravity and atmospheric drag as they ascend. They can achieve escape while their instantaneous speed is less than 11.2 km/s because they are adding energy over time and also gaining altitude, where the required escape velocity is lower.

Does the mass of the launched object affect the escape velocity?

No. As the formula v_esc = √(2GM/R) shows, the escape velocity depends only on the mass (M) and radius (R) of the planet, not on the mass of the projectile. This is because while a more massive object requires more energy to escape, it also has more inertia, and these two effects cancel exactly. In the simulator, you'll see all projectiles behave identically for the same launch speed.

What is the difference between achieving orbit and achieving escape velocity?

Achieving a stable orbit requires reaching a high horizontal speed (roughly 7.8 km/s for low Earth orbit) to continually fall around the planet. Escape velocity is a higher speed (about 11.2 km/s) directed away from the planet, which allows you to leave its sphere of influence entirely. Orbiting is about being captured by gravity, while escaping is about breaking free from it.

Escape Velocity

Launch from different planets and see trajectory results.

About this model

Escape velocity is the minimum speed an object must achieve to break free from a celestial body's gravitational pull without further propulsion. This simulator visualizes this fundamental concept by allowing you to launch a projectile from the surface of various planets and moons. The core physics is governed by Newton's law of universal gravitation and the conservation of mechanical energy. The gravitational force is given by F = G * (M * m) / r², where G is the gravitational constant, M is the planetary mass, m is the projectile mass, and r is the distance from the center. By setting the initial kinetic energy (½mv²) equal to the work needed to overcome gravity to an infinite distance, we derive the escape velocity formula: v_esc = √(2GM/R), where R is the planet's radius. The simulator simplifies reality by ignoring atmospheric drag, the rotation of the planet, and gravitational influences from other bodies, treating the launch as a radial path away from a perfectly spherical mass. By interacting, you will learn how a planet's mass and size directly determine its escape velocity, observe the distinct outcomes of sub-escape, escape, and orbital trajectories, and gain intuition for why leaving a massive, compact world like Earth is harder than leaving a smaller one like Mars.

Who it's for: High school and introductory college physics students studying Newtonian gravity, orbital mechanics, and energy conservation.

Key terms

Escape Velocity
Newton's Law of Universal Gravitation
Conservation of Energy
Gravitational Potential Energy
Kinetic Energy
Trajectory
Celestial Body
Orbital Mechanics

How it works

From distance r from the center of a spherical body, the escape speed is v_esc = √(2GM/r). Launch radially outward: below v_esc the probe stays bound (ellipse); at or above v_esc the specific mechanical energy is non-negative and the trajectory can reach infinity. Circular orbit speed √(GM/r) is smaller by √2 — compare the readouts. Planet presets scale GM and radius for a qualitative feel, not astronomical accuracy.

Key equations

E = ½v² − GM/r · escape when E ≥ 0

v_esc = √(2GM/r), v_circ = √(GM/r)

Frequently asked questions

If I reach escape velocity, does that mean I stop being pulled by the planet's gravity?: No. Gravity extends infinitely, so you are always pulled. Escape velocity is the speed where your kinetic energy is exactly equal to the negative gravitational potential energy. This means you have just enough speed to coast infinitely far away, slowing down continuously but never falling back. At any finite distance, gravity is still acting on you, just very weakly.
Why is the escape velocity for Earth about 11.2 km/s, but rockets don't need to reach that speed all at once?: The escape velocity formula assumes a single impulsive burst from the surface with no further thrust. Real rockets provide continuous thrust over minutes, fighting gravity and atmospheric drag as they ascend. They can achieve escape while their instantaneous speed is less than 11.2 km/s because they are adding energy over time and also gaining altitude, where the required escape velocity is lower.
Does the mass of the launched object affect the escape velocity?: No. As the formula v_esc = √(2GM/R) shows, the escape velocity depends only on the mass (M) and radius (R) of the planet, not on the mass of the projectile. This is because while a more massive object requires more energy to escape, it also has more inertia, and these two effects cancel exactly. In the simulator, you'll see all projectiles behave identically for the same launch speed.
What is the difference between achieving orbit and achieving escape velocity?: Achieving a stable orbit requires reaching a high horizontal speed (roughly 7.8 km/s for low Earth orbit) to continually fall around the planet. Escape velocity is a higher speed (about 11.2 km/s) directed away from the planet, which allows you to leave its sphere of influence entirely. Orbiting is about being captured by gravity, while escaping is about breaking free from it.

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Escape Velocity

About this model

How it works

Key equations

Frequently asked questions

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About this model

How it works

Key equations

Frequently asked questions