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HD 2638 b is a planet of the star HD 2638. It is a typical "hot Jupiter", a planet that orbits its parent star in a very tight "torch orbit". The distance to the star is less than 1/20 Earth's distance from the Sun. One orbital revolution lasts only about three and half days.
HD 16175 is a 7th magnitude G-type star with temperature about 6000 K located approximately 196 light-years away in the Andromeda constellation. This star is only visible through binoculars or better equipment; it is also 3.3 times more luminous, is 1.34 times more massive, and has a radius 1.66 times bigger than our local star.
HD 52265 b is a gas giant exoplanet located approximately 98 light-years away in the constellation of Monoceros, orbiting the star HD 52265. The planet has a minimum mass slightly more than that of Jupiter. Mean distance between the planet and the star is half that of Earth from the Sun. It was discovered by both the California and Carnegie Planet Search team and the Geneva Extrasolar Planet Search team independently of each other. By studying the fluctuations of the brightness of a host star, the inclination of the stars equator was determined. This allowed to calculate its true mass, assuming that the planet orbits in the plane of the star's equator.
HD 167042 b is a gas giant extrasolar planet located approximately 163 light-years away in the constellation of Draco, orbiting the star HD 167042. The mass 1.7 MJ is only minimum since the inclination of the orbital plane is unknown. As it is typical for most known extrasolar planets, it orbits less than 3 AU from the parent star, hence taking less than 2,000 days to revolve. For this planet, it orbits at 1.30 AU and taking 413 days to revolve around the star. Unlike most exoplanets, the eccentricity of the orbit is low, only 3%.
HD 16175 b is an extrasolar planet located approximately 195.6 light-years away in the constellation of Andromeda, orbiting the star HD 16175. This planet masses 4.8 times that of Jupiter. However, the mass is only a minimum since the inclination of the orbit is not known. This planet orbits at about 2.2 astronomical units, taking 2.73 years to revolve around the star. The orbit of the planet is highly noncircular with an eccentricity at 0.64.
HD 8574 b is an extrasolar planet discovered in 2001 by a team of European astronomers using Doppler spectroscopy as part of the ELODIE Planet Search Survey, and was published in a paper with five other planets. HD 8574 b is in the orbit of host star HD 8574. The planet is at most two times the mass of Jupiter, orbiting every 227 days at three quarters of the distance between the Earth and Sun. HD 8574 b has a very elliptical orbit, far more than that of Jupiter.
BD-10°3166 b is an extrasolar planet approximately 268 light-years away in the constellation of Crater. This planet is a so-called "Hot Jupiter," a planet that orbits its parent star in a very close orbit. Distance to the star is less than 1/20th Earth's distance from the Sun. No transits by the planet have been detected, so the planet's orbital plane cannot be exactly aligned with our direction of view.
HD 154672 b is an extrasolar planet located approximately 210 light-years away in the constellation of Ara, orbiting the metal-rich and aged star HD 154672. This planet has a minimum mass five times that of Jupiter and orbits at about 60% the distance between the Earth to the Sun. Its orbit is very elliptical, which causes temperatures on the planet to vary significantly as it proceeds along its orbit. This planet was discovered in Las Campanas Observatory on September 5, 2008 using the radial velocity method. Along with HD 205739 b, the planets were the first to be discovered by the N2K Consortium using the Magellan Telescopes.
HD 60532 b is an extrasolar planet located approximately 84 light-years away in the constellation of Puppis, orbiting the star HD 60532. This planet has a true mass of 3.15 times more than Jupiter, orbits at 0.77 AU, and takes 201.83 days to revolve in an eccentric orbit. This planet was discovered on September 22, 2008 in La Silla Observatory using the HARPS spectrograph. On this same day, the second planet in this system, HD 60532 c, was discovered in a 1:3 orbital resonance.
HD 147018 b is a gas giant extrasolar planet which orbits the G-type main sequence star HD 147018, located approximately 140 light years away in the constellation Triangulum Australe. This planet has minimum mass more than twice that of Jupiter but this planet orbits a lot closer to the star than Jupiter to the Sun by a factor of 22. Meanwhile, it has an eccentric orbit. The planet can get as close to the star as 0.13 AU or can get as far as 0.35 AU. Further out, there is another superjovian planet HD 147018 c, which was discovered on the same date as this planet, on August 11, 2009.
HD 147018 is a star in the southern constellation of Triangulum Australe. It has a yellow-orange hue with an apparent visual magnitude of 8.30, which is too faint to be seen with the naked eye but can be viewed with a small telescope. The star is located at a distance of 132 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −27.5 km/s.
HD 171238 is a 9th magnitude G-type main sequence star located approximately 146 light years away in the constellation Sagittarius. This star is a little bit cooler, less massive, older, and more metallic than the Sun. In August 2009, it was announced that this star has a planet.
HD 171238 b is an extrasolar planet which orbits the G-type main sequence star HD 171238, located approximately 164 light years away in the constellation Sagittarius. This planet has minimum mass two and a half times greater than Jupiter and orbits two times closer to the star than Jupiter to the Sun. However this planet orbits in an eccentric orbit, about two astronomical units difference between periastron and apastron distances. This planet was discovered in August 2009 by using the radial velocity method in La Silla Observatory, Chile.
HD 204313 is an 8th magnitude G-type main sequence star located approximately 155 light years away in the constellation Capricornus.
HD 204313 b is an extrasolar planet which orbits the G-type main sequence star HD 204313, located approximately 155 light years away in the constellation Capricorn. This planet orbits the star at a distance of 3.082 astronomical units and takes 1931 days or 5.29 years to revolve around the star. It has minimum mass four times that of Jupiter. However the radius and inclination are not known since this planet was not detected by transit method or direct imaging. Instead, this planet was detected by radial velocity method using the CORALIE Echelle spectrograph mounted on the 1.2 meter Euler Swiss Telescope located at La Silla Observatory in Atacama desert, Chile on August 11, 2009.
HD 190984 b is an extrasolar planet which orbits the F-type main sequence star HD 190984, located approximately 330 light years away in the constellation Pavo. This planet is at least three times more massive than Jupiter and takes 13 years and four-and-a-half months to orbit the star at a semimajor axis of 5.5 AU with an eccentricity of 0.57. This planet was detected by HARPS on October 19, 2009, together with 29 other planets.
HD 13931 b is an extrasolar planet which orbits the G-type star HD 13931, located approximately 155 light years away in the constellation Andromeda. This planet takes 11.55 years to orbit the star at the average distance of 5.15 AU or 770 Gm. The planet's eccentricity (0.02) is about the same as Earth. The orbital distance for this planet ranges from 5.05 to 5.25 AU. This planet was discovered by using radial velocity method from spectrograph taken at Keck Observatory on November 13, 2009.
HD 129445 b is an eccentric Jupiter gas giant exoplanet orbiting the star HD 129445 which was discovered by the Magellan Planet Search Program in 2010. Its mass is 1.6 times Jupiter's, and it takes 5 years to complete one orbit around HD 129445, a G-type star approximately 210 light years away.
HD 4313 b is an extrasolar planet orbiting the K-type star HD 4313 approximately 447 light years away in the constellation Pisces. This planet was discovered using the Doppler spectroscopy method.
An exoplanet is a planet located outside the Solar System. The first evidence of an exoplanet was noted as early as 1917, but was not recognized as such until 2016. No planet discovery has yet come from that evidence. However, the first scientific detection of an exoplanet began in 1988. Afterwards, the first confirmed detection came in 1992, with the discovery of several terrestrial-mass planets orbiting the pulsar PSR B1257+12. The first confirmation of an exoplanet orbiting a main-sequence star was made in 1995, when a giant planet was found in a four-day orbit around the nearby star 51 Pegasi. Some exoplanets have been imaged directly by telescopes, but the vast majority have been detected through indirect methods, such as the transit method and the radial-velocity method. As of 1 April 2021, there are 4,704 confirmed exoplanets in 3,478 systems, with 770 systems having more than one planet. This is a list of the most notable discoveries.
References
- Segransan; et al. (February 2010). "The CORALIE survey for southern extrasolar planets. XVI. Discovery of a planetary system around HD 147018 and of two long period and massive planets orbiting HD 171238 and HD 204313". Astronomy & Astrophysics . 511. article A45. arXiv: 0908.1479 . Bibcode:2010A&A...511A..45S. doi:10.1051/0004-6361/200912136.
Coordinates: 
16h 23m 00.1463s, −61° 41′ 19.542″
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