Exoplanet Radial Velocity Wobble

This simulation renders a full 3D star-planet system you can freely orbit, built from real two-body Kepler orbital mechanics: the planet and its host star both trace ellipses around their shared barycenter, sized in inverse proportion to their masses. As the star swings toward and away from Earth (off to the right of the scene) it is tinted blue when approaching and orange-red when receding — the Doppler shift that ground-based spectrographs measure as a radial-velocity curve, plotted live in the corner graph. Adjust planet mass, orbital distance, star mass and eccentricity to see how each reshapes the star's wobble radius, the orbital period and the radial-velocity semi-amplitude astronomers actually report.