Comparer des méthodes

	Méthode des vitesses radiales	Simulation N-corps
Domaine	Physique appliquée	Physique appliquée
Famille	Process / pipeline	Process / pipeline
Année d'origine	1844	1687
Auteur d'origine	Friedrich Wilhelm Bessel	Isaac Newton
Type	Spectroscopic measurement technique	Computational simulation algorithm
Source fondatrice	Mayor, M., & Queloz, D. (1995). A Jupiter-mass companion to a solar-type star. Nature, 378(6555), 355-359.	Poincaré, H. (1892). Les méthodes nouvelles de la mécanique céleste. Gauthier-Villars.
Alias	Doppler method, spectroscopic velocity measurement	gravitational N-body problem, many-body simulation
Apparentées	3	5
Résumé	The radial velocity method detects exoplanets by measuring the Doppler shift of a star's spectral lines caused by gravitational tugging from orbiting planets. When a planet orbits a star, the star wobbles slightly toward and away from Earth, creating periodic shifts in its light spectrum. First proposed by Friedrich Wilhelm Bessel in the 19th century and successfully applied to exoplanet detection in 1995, this method has discovered nearly half of all known exoplanets.	N-body simulation is a computational method for modeling the dynamics of a system of particles under mutual gravitational forces. Originating from Newton's laws of motion and gravitation, it solves the fundamental equations of celestial mechanics. This technique is essential for understanding planetary orbits, star cluster evolution, and cosmological structure formation.