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List Of Exoplanets Discovered Between 2000–2009
{{DEFAULTSORT:List of exoplanets discovered between 2000-2009 ...
This is a List of exoplanets discovered between 2000–2009. For exoplanets detected only by radial velocity, the mass value is actually a lower limit. (See Minimum mass for more information) Specific exoplanet lists References 2000-2009 exoplanets 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 recognized as such. The first confirmation of detection occurred in 1992. A different planet, init ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minimum Mass
In astronomy, minimum mass is the lower-bound calculated mass of observed objects such as planets, stars and binary systems, nebulae, and black holes. Minimum mass is a widely cited statistic for extrasolar planets detected by the radial velocity method or Doppler spectroscopy, and is determined using the binary mass function. This method reveals planets by measuring changes in the movement of stars in the line-of-sight, so the real orbital inclinations and true masses of the planets are generally unknown. This is a result of sin ''i'' degeneracy. If inclination ''i'' can be determined, the true mass can be obtained from the calculated minimum mass using the following relationship: M_\text = \frac Exoplanets Orientation of the transit to Earth Most stars will not have their planets lined up and orientated so that they eclipse over the center of the star and give the viewer on earth a perfect transit. It is for this reason that when we often are only able to extrapolate ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
The Astrophysical Journal
''The Astrophysical Journal'', often abbreviated ''ApJ'' (pronounced "ap jay") in references and speech, is a peer-reviewed Peer review is the evaluation of work by one or more people with similar competencies as the producers of the work (peers). It functions as a form of self-regulation by qualified members of a profession within the relevant field. Peer review ... scientific journal of astrophysics and astronomy, established in 1895 by American astronomers George Ellery Hale and James Edward Keeler. The journal discontinued its print edition and became an electronic-only journal in 2015. Since 1953 ''The Astrophysical Journal Supplement Series'' (''ApJS'') has been published in conjunction with ''The Astrophysical Journal'', with generally longer articles to supplement the material in the journal. It publishes six volumes per year, with two 280-page issues per volume. ''The Astrophysical Journal Letters'' (''ApJL''), established in 1967 by Subrahmanyan Chandrasekhar as ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
55 Cancri F
55 Cancri f (abbreviated 55 Cnc f), also designated Rho1 Cancri f and formally named Harriot , is an exoplanet approximately 41 light-years away from Earth in the constellation of Cancer (the Crab). 55 Cancri f is the fourth known planet (in order of distance) from the star 55 Cancri and the first planet to have been given the designation of "f". Name In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Harriot for this planet. The winning name was submitted by the Royal Netherlands Association for Meteorology and Astronomy of the Netherlands. It honors the astronomer Thomas Harriot. Discovery The initial presentation of this planet occurred at a meeting of the American Astronomical Society in April 2005, however it was another two and a half years befo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
55 Cancri E
55 Cancri e (abbreviated 55 Cnc e, formally named Janssen and nicknamed "Hell on Earth") is an exoplanet in the orbit of its Sun-like host star 55 Cancri A. The mass of the exoplanet is about 8.63 Earth masses and its diameter is about twice that of the Earth, thus making it the first super-Earth discovered around a main sequence star, predating Gliese 876 d by a year. It takes fewer than 18 hours to complete an orbit and is the innermost-known planet in its planetary system. 55 Cancri e was discovered on 30 August 2004. However, until the 2010 observations and recalculations, this planet had been thought to take about 2.8 days to orbit the star. In October 2012, it was announced that 55 Cancri e could be a carbon planet. In February 2016, it was announced that NASA's Hubble Space Telescope had detected hydrogen and helium (and suggestions of hydrogen cyanide), but no water vapor, in the atmosphere of 55 Cancri e, the first time the atmosphere of a super-Earth exoplanet was a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
55 Cancri D
55 Cancri d (abbreviated 55 Cnc d), formally named Lipperhey , is an extrasolar planet in a long-period orbit around the Sun-like star 55 Cancri A. Located at a similar distance from its star as Jupiter is from the Sun, it is the fifth and outermost known planet in its planetary system. 55 Cancri d was discovered on June 13, 2002. Name In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Lippershey for this planet.Final Results of NameExoWorlds Public Vote Released International Astronomical Union, 15 December 2015. The winning name was submitted by the Royal Neth ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
55 Cancri C
55 Cancri c (abbreviated 55 Cnc c), formally named Brahe (pronounced or ), is an extrasolar planet in an eccentric orbit around the Sun-like star 55 Cancri A, making one revolution every 44.34 days. It is the third known planet in order of distance from its star. 55 Cancri c was discovered on June 13, 2002, and has a mass roughly half of Saturn. In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Brahe for this planet. The winning name was submitted by the Royal Netherlands Association for Meteorology and Astronomy of the Netherlands. It honors the astronomer Tycho Brahe. Discovery Like the majority of known extrasolar planets, 55 Cancri c was detected by observing changes in its star's radial velocity. This was achieved by making sensitive measurem ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
54 Piscium B
54 Piscium b (HD 3651 b), occasionally catalogued as 54 Piscium Ab to differentiate from the brown dwarf in the system, is an extrasolar planet approximately 36 light-years away in the constellation of Pisces (constellation), Pisces. It was discovered orbiting the K-type main sequence star, orange dwarf star 54 Piscium. Its minimum mass is one-fifth that of Jupiter, and it orbits the star in a very eccentricity (orbit), eccentric orbit about every two months. Discovery On January 16, 2003, a team of astronomers (led by Geoff Marcy) announced the discovery of an extrasolar planet around 54 Piscium using the radial velocity method, a process utilizing the "wobbling" effect that a star may experience if something is tugging on it. The planet has been estimated to have a mass of only 20 percent that of Jupiter (making the planet around the same size and mass of Saturn). Orbit and mass The planet orbits its sun at a distance of 0.28 astronomical units (which would be within the orbi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
47 Ursae Majoris D
47 Ursae Majoris d (sometimes abbreviated 47 Uma d) is an extrasolar planet approximately 46 light-years away in the constellation of Ursa Major. The planet was discovered located in a long-period orbit (38 years) around the star 47 Ursae Majoris. As of 2011, it is the outermost of three known planets in its planetary system. It has a mass of at least 1.64 times that of Jupiter. It is the longest-period planet detected by Doppler spectroscopy Doppler spectroscopy (also known as the radial-velocity method, or colloquially, the wobble method) is an indirect method for finding extrasolar planets and brown dwarfs from radial-velocity measurements via observation of Doppler shifts in t .... The evidence of this planet was found by Bayesian Kepler periodogram in March 2010. References * 47 Ursae Majoris Exoplanets discovered in 2010 Giant planets Exoplanets detected by radial velocity {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
47 Ursae Majoris C
47 Ursae Majoris c (abbreviated 47 UMa c), formally named Taphao Kaew , is an extrasolar planet approximately 46 light-years from Earth in the constellation of Ursa Major. The planet was discovered located in a long-period around the star 47 Ursae Majoris. Its orbit lasts 6.55 years and the planet has a mass at least 0.540 times that of Jupiter. Name In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Taphao Kaew ( th, ตะเภาแก้ว ) for this planet. The winning name was submitted by the Thai Astronomical Society of Thailand. Taphaokaeo was one of two sisters associated with a Thai folk tale. Discovery Like many known extrasolar planets at the time, 47 Ursae Majoris c was discovered by detecting changes in its star's radial velocity caused b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
42 Draconis B
42 Draconis b (abbreviated 42 Dra b), formally named Orbitar , is a candidate extrasolar planet located approximately 315 light years from Earth in the constellation of Draco. It orbits the 5th magnitude K-type giant star 42 Draconis with a period of 479 days and 38% orbital eccentricity. The planet was discovered using the radial velocity method on March 20, 2009. Following its discovery the planet was designated 42 Draconis b. In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning name was Orbitar for this planet. The winning name was submitted by the Brevard Astronomical Society of Brevard County, Florida, United States. Orbitar is a contrived word paying homage to the space launch and orbital operations of NASA. A 2021 study found that more recent radial velocity m ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
41 Lyncis B
41 Lyncis b (abbreviated 41 Lyn b), also designated HD 81688 b and named Arkas , is an extrasolar planet approximately 280 light-years from Earth in the constellation of Ursa Major. A gas giant with a minimum mass 2.7 times that of Jupiter, it orbits the K-type star 41 Lyncis with an orbital period of 184 days (corresponding to a semi-major axis of 0.81 AU). It was discovered and announced by Bun'ei Sato on February 19, 2008. Name In July 2014, the International Astronomical Union (IAU) launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the name Arkas for this planet. The winning name was submitted by the Okayama Astro Club of Japan. Arkas was the son of Callisto (Ursa Major) in Greek mythology. See also * 18 Delphini b * Xi Aquilae b Xi Aquilae b (abbreviated ξ Aquilae b, ξ Aql b), formally named Fortitudo , is an extraso ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
30 Arietis Bb
30 Arietis (abbreviated 30 Ari) is a 6th- apparent-magnitude multiple star system in the constellation of Aries. ''30 Arietis'' is the Flamsteed designation. 30 Arietis A and B are separated by or about at a distance of 130 light years away. The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores. The 30 Arietis system is 910 million years old, one fifth the age of the Sun. Star system 30 Arietis A and B are separated by 38.1", corresponding to 1,500 AU at a distance of 130 light years. The pair are at almost the same distance, have very similar proper motions, and are considered almost certain to be gravitationally bound with a likely period around 34,000 years. The main components of both systems are both binaries with a composite spectra belonging to F-type main-sequence stars, meaning they are fusing hydrogen in their cores. 30 Arietis A is a s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
