List of exoplanets discovered in 2018 (306).List of exoplanets discovered in 2017 (158).List of exoplanets discovered in 2016 (1513).List of exoplanets discovered in 2015 (151).List of exoplanets discovered in 2014 (878).List of exoplanets discovered in 2013 (151).List of exoplanets discovered in 2012 (149).List of exoplanets discovered in 2011 (179). List of exoplanets discovered in 2010 (109).List of exoplanets discovered between 2000–2009 (379).List of exoplanets discovered before 2000 (32).Specific exoplanet lists ĭistribution of confirmed exoplanets vis-à-vis distance from Solar System Features in the disks may suggest the presence of planets, though this is not considered a definitive detection method. The dust can be detected because it absorbs starlight and re-emits it as infrared radiation. ĭisks of space dust surround many stars, thought to originate from collisions among asteroids and comets. No new planets have been discovered with this method although a few already discovered planets have been detected with this method. With polarimetry method, a polarized light reflected off the planet is separated from unpolarized light emitted from the star. This causes the brightness of the star to slightly deviate depending how it is rotated relative to Earth. Massive planets close to their host stars can slightly deform the shape of the star. The brightness of the star changes as the planet moves closer or further away from its host star. Relativistic beaming measures the observed flux from the star due to its motion. As the planet orbits around the star, the amount of light changes due to planets having phases from Earth's viewpoint or planet glowing more from one side than the other due to temperature differences. When a planet orbits very close to the star, it catches a considerable amount of starlight. As of 2013, a few planets have been discovered with this method. Deviations from the periodicity can sometimes be caused by a planet orbiting it. Like pulsars, there are some other types of stars which exhibit periodic activity. Variable star timing (pulsation frequency).But as of 2011, it has not been very productive five planets have been detected in this way, around three different pulsars. The first confirmed discovery of an extrasolar planet was made using this method. If planets orbit the pulsar, they will cause slight anomalies in the timing of its observed radio pulses. It has produced only a few disputed detections, though it has been successfully used to investigate the properties of planets found in other ways.Ī pulsar (the small, ultradense remnant of a star that has exploded as a supernova) emits radio waves extremely regularly as it rotates. Because the motion is so small, however, this method has not yet been very productive. The motion of a star due to the gravitational influence of a planet may be observable. Unlike most other methods which have detection bias towards planets with small (or for resolved imaging, large) orbits, microlensing method is most sensitive to detecting planets around 1–10 AU away from Sun-like stars.Īstrometry consists of precisely measuring a star's position in the sky and observing the changes in that position over time. Planets orbiting the lensing star can cause detectable anomalies in the magnification as it varies over time. Microlensing occurs when the gravitational field of a star acts like a lens, magnifying the light of a distant background star. Although no new planets or moons have been discovered with this method, it is used to successfully confirm many transiting circumbinary planets. Other naming systems exist.Īnimation showing difference between planet transit timing of one-planet and two-planet systems When a planet orbits multiple stars or if the planet has moons, its transit time can significantly vary per transit. A limited number of exoplanets have IAU-sanctioned proper names. A provisional IAU-sanctioned standard exists to accommodate the designation of circumbinary planets. If several planets in the same system are discovered at the same time, the closest one to the star gets the next letter, followed by the other planets in order of orbital size. Letters are given in order of each planet's discovery around the parent star, so that the first planet discovered in a system is designated "b" (the parent star is considered to be "a") and later planets are given subsequent letters. For exoplanets orbiting a single star, the IAU designation is formed by taking the designated or proper name of its parent star, and adding a lower case letter. The convention for designating exoplanets is an extension of the system used for designating multiple-star systems as adopted by the International Astronomical Union (IAU). Main article: Exoplanet naming convention
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