physics

Planetary Science & Solar System

Explore the physics of planets and moons — atmospheric scale heights, tidal heating of volcanic worlds, impact crater formation, Roche limit disruption, and planetary energy balance from albedo and greenhouse effects.

planetary sciencesolar systematmospheretidal heatingimpact cratersRoche limitalbedoastrophysics

Planetary science sits at the intersection of physics, chemistry, and geology, applying fundamental laws to understand worlds beyond our own. From the towering volcanoes of Io driven by tidal flexing to the delicate energy balance that sets a planet's surface temperature, every body in the Solar System is a natural laboratory for testing physical principles at extreme scales.

These simulations let you model atmospheric escape, tidal dissipation in moons, impact cratering mechanics, gravitational disruption limits, and planetary thermal equilibrium — all with interactive controls grounded in the equations used by NASA mission scientists and planetary researchers worldwide.

5 interactive simulations

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Albedo & Planetary Energy Balance

Calculate equilibrium temperature from stellar luminosity, orbital distance, albedo, and greenhouse effect — understand why Venus is hotter than Mercury despite being farther from the Sun

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Impact Crater Scaling: Size vs Energy

Calculate impact crater diameter from impactor size, velocity, and target properties — explore the physics of hypervelocity impacts that shaped planetary surfaces

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Planetary Atmosphere: Scale Height & Escape Velocity

Model atmospheric structure using scale height and compare thermal velocity to escape velocity — understand why Mars lost its atmosphere while Earth kept its own

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Roche Limit: Tidal Disruption Distance

Calculate the Roche limit — the critical distance where tidal forces tear apart a satellite — and visualize the disruption process that creates planetary rings

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Tidal Heating & Io-Style Dissipation

Simulate tidal heating in moons like Io — explore how orbital eccentricity, distance, and interior rigidity drive volcanic activity through gravitational flexing