Comparer des méthodes

	Méthode des vitesses radiales	Analyse de courbe de lumière
Domaine	Physique appliquée	Physique appliquée
Famille	Process / pipeline	Process / pipeline
Année d'origine	1844	1880
Auteur d'origine	Friedrich Wilhelm Bessel	Edward Pickering
Type	Spectroscopic measurement technique	Signal processing and astronomical observation technique
Source fondatrice	Mayor, M., & Queloz, D. (1995). A Jupiter-mass companion to a solar-type star. Nature, 378(6555), 355-359.	Ricker, G. R., et al. (2015). TESS: Transiting Exoplanet Survey Satellite. Journal of Astronomical Telescopes, Instruments, and Systems, 1(1), 014003.
Alias	Doppler method, spectroscopic velocity measurement	photometric analysis, transit photometry, eclipsing binary analysis
Apparentées	3	3
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.	Light curve analysis is the study of the brightness variation of a celestial object over time, used to detect and characterize exoplanets, eclipsing binaries, and variable stars. When a planet transits in front of its host star, the star's brightness dips slightly. By analyzing these photometric signatures, astronomers can determine planetary radii, orbital periods, and atmospheric properties. This method has discovered thousands of exoplanets and revealed the structure of stellar systems.