Skip to main content
Physics Fundamentals

Orbital
Mechanic

Launch satellites into stable orbits.
Real gravity. Real Kepler's laws. 8 levels.

Click anywhere to begin
🛸 Orbital Physics Game

Orbital Mechanic — The Free Online Orbital Physics Game

Orbital Mechanic is a free physics game that teaches orbital velocity, Kepler's laws, and gravitational mechanics through 8 levels of satellite launch puzzles. Discover why satellites stay up — not by reading, but by doing.

How to play

  1. 1
    Click to set your launch point: Click anywhere near the planet surface. Your satellite launches from the point on the planet closest to your click.
  2. 2
    Drag to set velocity: Drag away from your launch point. Drag direction sets velocity direction — drag distance sets speed.
  3. 3
    Find stable orbit: When your satellite enters the target orbit band (shown as a cyan ring), a progress arc appears. Hold the orbit for 3.5 seconds to achieve it.
  4. 4
    Watch for crashes and escapes: Too little velocity and you crash into the planet. Too much and you escape into space. The sweet spot is orbital velocity.
  5. 5
    Earn stars: Fewer launches = more stars. Par is shown per level — 3 stars means you matched or beat par.

The physics behind the game

Orbital velocity

v = √(GM/r)

For a circular orbit, gravity must exactly provide the centripetal force. This gives a single unique speed at every radius — too fast and the satellite spirals out, too slow and it falls inward.

Kepler's third law

T² = (4π²/GM)·r³

The orbital period scales with r^(3/2). Double the orbital radius and the period increases by 2^(3/2) ≈ 2.83×. This is why geostationary satellites must orbit at a specific altitude.

Escape velocity

v_esc = √(2GM/r)

Escape velocity is exactly √2 times the circular orbital velocity at the same radius. Launch faster than this and your satellite never returns.

Gravitational potential energy

U = −GMm/r

Orbital energy is always negative — the satellite is bound to the planet. As radius increases, energy increases (becomes less negative) and orbital velocity decreases.

Related articles

Orbital Mechanics and Kepler's Laws

Orbital Velocity: v = √(GM/r)

Gravity provides centripetal force: GMm/r² = mv²/r → v = √(GM/r). Higher orbits move slower: LEO (400 km) at 7.66 km/s; GEO (35,786 km) at 3.07 km/s; Moon at 1.02 km/s. Period: T = 2πr/v = 2π√(r³/GM) — Kepler's Third Law (T² ∝ r³). Geostationary orbit: T = 24 h → r = (GM_Earth × T²/4π²)^(1/3) = 42,164 km from Earth's centre. Used for TV satellites, weather monitoring, GPS (MEO).

Kepler's Three Laws

First: orbits are ellipses with the central body at one focus (circles are special case, eccentricity e = 0). Second: equal areas in equal times (conservation of angular momentum — gravity is a central force with no torque). Third: T² ∝ a³ (a = semi-major axis). For same central body: T² = (4π²/GM) a³. This lets us measure any mass: knowing orbital T and a gives M = 4π²a³/(GT²). We know the Sun's mass, all planet masses, and even galaxy masses this way.

Escape Velocity: v_esc = √(2GM/R)

Minimum speed to escape gravity from surface radius R: ½mv² = GMm/R → v_esc = √(2GM/R). Earth: 11.2 km/s. Moon: 2.4 km/s (why lunar lander ascent stage can escape easily with a small engine). Jupiter: 59.5 km/s. Black holes: v_esc > c — even light cannot escape from within the event horizon (Schwarzschild radius r_s = 2GM/c²). Rockets don't need to reach this speed instantly — they can escape via a continuous burn at lower speed.

Physics Fundamentals

Channel · Updates only

👋 Get concise physics updates — new articles, calculators, and tools. Your number stays private. No spam. No group chats. Just worthy content.

Your number is never shared or visible to others

Join the Channel