🚀

Aerospace Engineering & Orbital Mechanics

From Newton's cannonball to a Hohmann transfer orbit — gravity shapes everything in space. Explore gravitational dynamics, multi-body chaos, binary star systems and the clockwork precision of our solar system.

8 simulations Three.js · Canvas 2D Kepler · N-Body · Verlet

Aerospace & Orbital Mechanics is the science of how vehicles fly through the atmosphere and how spacecraft move under gravity. This category covers the full journey — from a rocket fighting gravity on the launch pad, through the Tsiolkovsky equation and staging, to Keplerian orbits, Hohmann transfers, the chaotic N-body problem, atmospheric re-entry heating and aerodynamic lift on a wing. By adjusting parameters such as specific impulse, mass ratio, entry angle, eccentricity and angle of attack in real time, you build genuine intuition for astrodynamics and aerodynamics rather than memorising formulae. These ideas underpin everything from satellite constellations and interplanetary missions to commercial aircraft design and planetary-defence strategies. Whether you are a student, an educator or simply curious about spaceflight, each interactive model turns abstract equations into something you can see, tweak and understand.

Category Simulations

Gravity at every scale — from binary stars to solar systems

Orbital mechanics is Newton's law of gravitation taken seriously. Two bodies follow perfect conics; add a third and chaos emerges. The N-body problem has no general closed-form solution — every planetary forecast is a numerical integration racing against accumulating error.

✈️
★★★ Advanced New
Supersonic Flow
Watch the Mach cone μ=arcsin(1/M) and oblique/bow shocks form as Mach number rises, with Rankine-Hugoniot pressure and density jumps and regime classification.
SupersonicMach ConeShock WaveCanvas 2D
🛩️
★★★ Advanced New
Wind Tunnel
Potential-flow streamlines over an aerofoil, cylinder or flat plate with pressure colouring Cp=1−(v/U)², stagnation points and circulation giving lift L=ρUΓ. Raise the angle of attack to stall.
Potential FlowLiftKutta-JoukowskiCanvas 2D
🌍
★★☆ Moderate
Solar System
All eight planets plus dwarf planets orbiting the Sun with real semi-major axes, eccentricities and inclinations. Toggle orbit trails, scale the distances logarithmically, and fast-forward centuries to watch resonances and conjunctions align.
Three.js Keplerian Orbits Eccentricity Log Scale
🛸
★★☆ Moderate
Orbital Mechanics Sandbox
Interactive 2D orbital simulator — launch a spacecraft, fire retrograde burns, demonstrate Hohmann transfers, and explore Lagrange points in the Earth-Moon system. Δv budget shown in real time.
Canvas 2D Hohmann Transfer Δv Budget Lagrange Points
★★☆ Moderate
Binary Star System
Two gravitationally bound stars orbiting their common barycentre. Adjust mass ratio from equal twins to extreme (neutron star + giant) and watch the orbit morph from circular to highly eccentric. Add a test particle to reveal chaotic regions.
Canvas 2D Barycentre Mass Ratio Eccentricity
🌌
★★★ Advanced
N-Body Gravity
Direct O(N²) gravitational simulation with Velocity Verlet integration and softened potential to avoid singularities. Spawn hundreds of bodies and watch galaxy-like structures, ejections and three-body choreographies emerge.
Canvas 2D Velocity Verlet Softening Barnes-Hut
🚀
★★☆ Moderate
Rocket Launch (Tsiolkovsky)
Two-stage rocket with live Tsiolkovsky Δv budget. Adjust specific impulse, propellant fraction and payload mass — see how mass ratio and staging determine whether you reach Low Earth Orbit.
Canvas 2D Tsiolkovsky Staging Gravity Turn
🔥
★★★ Advanced
Atmospheric Re-entry
Capsule descends from LEO at 7 800 m/s. Entry angle determines survival: too shallow and it skips out; too steep and aerodynamic heating and g-forces become lethal. Compare ballistic vs lifting trajectories.
Canvas 2D Drag Heating Entry Angle
🛸
New ★★☆ Moderate
Orbital Maneuvers
Plan a two-burn Hohmann transfer between circular Earth orbits. Use the vis-viva equation to compute Δv budgets and transfer times. Watch the animated spacecraft arc from LEO to GEO.
Canvas 2D Hohmann Δv Budget Vis-Viva
🌕
New ★★☆ Moderate
Moon Landing
Fly an Apollo-style lunar module to a soft touchdown. Manage throttle and gimbal with real Isp = 311 s and Moon gravity 1.62 m/s². Land on the pad — or crater the surface.
Canvas 2D Apollo Isp Lunar Gravity
✈️
New ★★☆ Moderate
NACA Airfoil
Generate any NACA 4-digit wing profile and visualise lift, drag and pressure distribution using thin airfoil theory. Tune camber, thickness and angle of attack — watch stall happen in real time.
Canvas 2D NACA Aerodynamics Thin Airfoil Theory
☄️
New ★★☆ Moderate
Asteroid Deflection
Fire a kinetic impactor at an Earth-crossing asteroid and watch RK4 orbital mechanics redirect its path. Choose Δv, direction and launch timing — will it miss Earth?
Canvas 2D Orbital Mechanics Kinetic Impactor Planetary Defense
☀️
New ★★☆ Moderate
Solar Sail
Photon radiation pressure spirals a reflective sail outward from Earth orbit. RK4 integration in AU/year units. Adjust area, mass and pitch angle to escape the inner solar system.
Canvas 2D RK4 Photon Pressure Orbital Mechanics

Key Concepts

The mathematics of spaceflight

Kepler's Laws
Orbits are ellipses with the central body at one focus; equal areas swept in equal times (conservation of angular momentum); period² ∝ semi-major axis³.
Tsiolkovsky Equation
Δv = Isp·g₀·ln(m₀/m_f). Specific impulse (Isp) and mass ratio completely determine a rocket's capability. This is why staging exists — discarding empty tanks increases mass ratio.
Hohmann Transfer
The most fuel-efficient two-impulse manoeuvre between circular coplanar orbits. Two burns tangent to the orbit change apoapsis and periapsis with minimum Δv expenditure.
Lagrange Points
Five equilibrium positions in a two-body system where gravitational and centrifugal forces balance. L4 and L5 are stable (Trojan asteroids); L1, L2, L3 are unstable saddle points.

Learning Resources

Explore orbital mechanics in depth

Neighbouring disciplines in physics and engineering

About Aerospace Engineering Simulations

Orbital rockets, atmospheric flight, aerodynamics, and re-entry — modelled

Aerospace engineering simulations model the physics of vehicles operating at the extremes of speed and altitude. Orbital mechanics simulators compute Hohmann transfer orbits, gravity assists, and orbital rendezvous procedures using two-body Keplerian dynamics and three-body perturbation theory. Rocket staging models calculate Δv budgets from the Tsiolkovsky rocket equation across multiple stages and propellant types.

Aerodynamics simulations model lift-to-drag polar curves for airfoil profiles and compute pressure distributions at varying angle-of-attack and Mach number using panel-method discretisation. Re-entry heating simulations model stagnation-point heat flux as a function of velocity and altitude, explaining the design requirements for heat shields. These models reflect the mathematical core of aerospace engineering education and are used in conceptual design and mission-planning tools.

Each simulation in this category is built with accuracy and interactivity in mind. The underlying mathematical models are the same ones used in academic research and professional engineering — just made accessible through a web browser. Changing parameters in real time and observing the results is one of the most effective ways to build intuition for complex scientific and engineering concepts.

Frequently Asked Questions

Common questions about this simulation category

What is the Tsiolkovsky rocket equation and why does it matter?
The Tsiolkovsky equation Δv = Isp·g₀·ln(m₀/m_f) relates a rocket's achievable velocity change to its exhaust velocity (specific impulse Isp) and mass ratio m₀/m_f. Because propellant mass dominates, even small increases in Isp dramatically improve Δv — which is why staging exists. The Rocket Launch simulation lets you adjust Isp, propellant fraction, and payload to see whether you reach Low Earth Orbit.
What is a Hohmann transfer orbit?
A Hohmann transfer is the most fuel-efficient two-impulse manoeuvre between circular coplanar orbits. The first burn raises the apoapsis to the target orbit; the second circularises at the apoapsis. The vis-viva equation v = √(GM(2/r − 1/a)) gives the required speeds at each point. You can plan and execute transfers interactively in the Orbital Maneuvers simulation.
How does atmospheric re-entry heating work?
At re-entry speeds (~7.8 km/s from LEO), air cannot flow around the capsule fast enough and instead compresses into a shockwave, heating it to thousands of degrees. Stagnation-point heat flux scales roughly as q ∝ ρ^0.5 · v³. Entry angle is critical: too shallow and the capsule skips out; too steep and aerodynamic heating and g-forces become lethal — both outcomes are modelled in the Atmospheric Re-entry simulation.
What generates lift on an aerofoil?
Lift arises from circulation: the aerofoil's camber and angle of attack force air to travel faster over the upper surface than the lower, creating a pressure difference (Bernoulli). The Kutta-Joukowski theorem gives lift per unit span L = ρUΓ, where Γ is the circulation. The NACA Airfoil simulation lets you tune camber, thickness, and angle of attack, and watch pressure distribution and stall onset in real time.

Every Aerospace & Orbital Mechanics simulation in this collection runs live in your browser, letting you explore an interactive Aerospace & Orbital Mechanics model without any installation or sign-up. From rocket staging and Hohmann transfers to re-entry heating and aerofoil lift, these tools make it easy to learn Aerospace & Orbital Mechanics online at your own pace. The same equations power real-world applications such as launching and de-orbiting satellites, planning interplanetary missions, designing heat shields and aircraft wings, and modelling asteroid-deflection strategies for planetary defence — proof that the physics on screen shapes the spacecraft and aircraft that fly above us today.