Gravitation & celestial motion
F = GMm/r²; vis-viva v² = GM(2/r − 1/a); Kepler's third law T² = 4π²a³/(GM).
Curved motion & gravitation (senior)Composition, projectile, centripetal force, orbits.
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Gravitation & celestial motion
Gravitation: a planet orbiting a star with Kepler's laws. This “Gravitation & celestial motion” page is an MVP interactive sketch — formulas, controls, and live readouts in the browser; a fuller bench may follow.
Gravitation: a planet orbiting a star with Kepler's laws.
Key formulas
F=\frac{GMm}{r^2}v=\sqrt{\frac{GM}{r}}T^2=\frac{4\pi^2}{GM}r^3
How to use
- Adjust parameters in the left panel.
- Use play / pause and speed controls.
- Match right-side readouts to the formulas.
- Reset to return to the initial state.
Applications
- Gravitation & celestial motion: Gravitation: a planet orbiting a star with Kepler's laws.
- Classroom focus: Kepler's third law T² = 4π²a³/(GM).
FAQ
What does MVP mean on this page?
An interactive sketch with formulas and parameters. Polished Ready labs are the full bench experience.
What does the “Gravitation & celestial motion” lab practice?
Tune parameters and match readouts to the “Gravitation & celestial motion” relations — useful for prep and demos.
Is force always along velocity?
No. Net force aligns with acceleration; velocity can point elsewhere.
How do graphs show uniform vs accelerated motion?
Uniform: constant x–t slope. Constant a: straight v–t with slope a.