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The first successful detection of an extrasolar planet using this method came in 2008, when HD 189733 b, a planet discovered three years earlier, was detected using polarimetry. [88] However, no new planets have yet been discovered using this method.
Astrometry has been used to discover a handful number of exoplanets, mostly gas giants more massive than Jupiter. It is based on measuring a star's proper motion, and seeing how that position changes over time: a planet with a sufficiently large mass is able to gravitationally pull its host star, making its proper motion vary over large timescales.
Exoplanets categorized by method of detection, including radial velocity, transit, gravitational microlensing, timing, and direct imaging. Properties (mass and semimajor axis) of planets color coded (see figure description page for key) by discovery method, with selected planets labeled, compared (light gray circles) with Solar System planets.
An exoplanet or extrasolar planet is a planet outside the Solar System. The first possible evidence of an exoplanet was noted in 1917 but was not then recognized as such. The first confirmed detection of an exoplanet was in 1992 around a pulsar, and the first detection around a main-sequence star was in 1995. A different planet, first detected ...
The Exoplanet Archive contains objects discovered through all methods (radial velocity, transits, microlensing, imaging, astrometry, eclipse timing variations, and transit timing variations/TTV) that have publicly available planetary parameters, with a mass (or minimum mass) equal to or less than 30 Jupiter masses.
Motion interpolation of seven images of the HR 8799 system taken from the W. M. Keck Observatory over seven years, featuring four exoplanets. This is a list of extrasolar planets that have been directly observed, sorted by observed separations. This method works best for young planets that emit infrared light and are far from the glare of the star.
Most known extrasolar planet candidates have been discovered using indirect methods and therefore only some of their physical and orbital parameters can be determined. For example, out of the six independent parameters that define an orbit, the radial-velocity method can determine four: semi-major axis , eccentricity , longitude of periastron ...
The following is a list of 456 extrasolar planets that were only detected by radial velocity method –– 31 confirmed and 323 candidates, sorted by orbital periods. Since none of these planets are transiting or directly observed, they do not have measured radii and generally their masses are only minimum.