81 Ceti B
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81 Ceti B
81 Ceti b (abbreviated 81 Cet b) is an extrasolar planet approximately 331 light years away in the constellation of Cetus. It is estimated to be 5.3 times the mass of Jupiter which also makes it a gas giant. It orbits the G-type giant star 81 Ceti at an average distance of 2.5 AU, taking about 2.6 years to revolve with an eccentricity of 20.6. Discovery The preprint announcing this planet was submitted to the arXiv electronic repository on July 2, 2008, by Bun'ei Sato and collaborators, who discovered it using the Doppler Spectroscopy method, during the Okayama Planet Search radial velocity survey of G and K giants at Okayama Astrophysical Observatory. See also * 14 Andromedae b * 6 Lyncis b 6 Lyncis b (abbreviated 6 Lyn b) is an extrasolar planet orbiting the K-type subgiant star 6 Lyncis which is approximately 182 light years away in the Lynx constellation. The planet has a minimum mass . The orbital period for this planet is 8 ... * 79 Ceti b * 94 Ceti b ...
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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 the spectrum of the planet's parent star. 1,018 extrasolar planets (about 19.5% of the total) have been discovered using Doppler spectroscopy, as of November 2022. History Otto Struve proposed in 1952 the use of powerful spectrographs to detect distant planets. He described how a very large planet, as large as Jupiter, for example, would cause its parent star to wobble slightly as the two objects orbit around their center of mass. He predicted that the small Doppler shifts to the light emitted by the star, caused by its continuously varying radial velocity, would be detectable by the most sensitive spectrographs as tiny redshifts and blueshifts in the star's emission. However, the technology of the time produced radial-velocity meas ...
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Okayama Planet Search Program
The Okayama Planet Search Program (OPSP) was started in 2001 with the goal of spectroscopically searching for planetary systems around stars. It reported on the detection of 3 new extrasolar planets: (18 Delphini b, Xi Aquilae b, xi Aql b, and 41 Lyncis b), around intermediate-mass G and K star, K giants 18 Delphini, Xi Aquilae, and HD 81688. Also, it updated the orbital parameters of HD 104985 b, the first planet discovered around the G star, G giants from the survey, by using the data collected during the past six years. Since 2001, it has been conducting a precise Doppler effect, Doppler Astronomical survey, survey of about 300 G and K giants using a 1.88m telescope, the High Dispersion Echelle Spectrograph (HIDES), and an iodine absorption cell I2 cell at the Okayama Astrophysical Observatory (OAO). Discoveries * Observatory * Okayama Astrophysical Observatory, Kurashiki in Japan References

* * * * Exoplanet search projects {{astrobiology-stub ...
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Giant Planets
The giant planets constitute a diverse type of planet much larger than Earth. They are usually primarily composed of low-boiling-point materials (volatiles), rather than rock or other solid matter, but massive solid planets can also exist. There are four known giant planets in the Solar System: Jupiter, Saturn, Uranus and Neptune. Many extrasolar giant planets have been identified orbiting other stars. They are also sometimes called jovian planets, after Jupiter ("Jove" being another name for the Roman god "Jupiter"). They are also sometimes known as gas giants. However, many astronomers now apply the latter term only to Jupiter and Saturn, classifying Uranus and Neptune, which have different compositions, as ice giants. Both names are potentially misleading: all of the giant planets consist primarily of fluids above their critical points, where distinct gas and liquid phases do not exist. The principal components are hydrogen and helium in the case of Jupiter and Saturn, and ...
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Cetus (constellation)
Cetus () is a constellation, sometimes called 'the whale' in English. The Cetus was a sea monster in Greek mythology which both Perseus and Heracles needed to slay. Cetus is in the region of the sky that contains other water-related constellations: Aquarius, Pisces and Eridanus. Features Ecliptic Cetus is not among the 12 true zodiac constellations in the J2000 epoch, nor classical 12-part zodiac. The ecliptic passes less than 0.25° from one of its corners. Thus the moon and planets will enter Cetus (occulting any stars as a foreground object) in 50% of their successive orbits briefly and the southern part of the sun appears in Cetus for about one day each year. Many asteroids in belts have longer phases occulting the north-western part of Cetus, those with a slightly greater inclination to the ecliptic than the moon and planets. As seen from Mars, the ecliptic (apparent plane of the sun and also the average plane of the planets which is almost the same) passes into it. ...
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Extrasolar Planets Encyclopaedia
The Extrasolar Planets Encyclopaedia is an astronomy website, founded in Paris, France at the Meudon Observatory by Jean Schneider in February 1995, which maintains a database of all the currently known and candidate extrasolar planets, with individual pages for each planet and a full list interactive catalog spreadsheet. The main catalogue comprises databases of all of the currently confirmed extrasolar planets as well as a database of unconfirmed planet detections. The databases are frequently updated with new data from peer-reviewed publications and conferences. In their respective pages, the planets are listed along with their basic properties, including the year of planet's discovery, mass, radius, orbital period, semi-major axis, eccentricity, inclination, longitude of periastron, time of periastron, maximum time variation, and time of transit, including all error range values. The individual planet data pages also contain the data on the parent star, including name, di ...
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94 Ceti B
94 Ceti b or 94 Ceti Ab to distinguish it from the distant red dwarf companion, is an extrasolar planet orbiting its star once every 1.2 years. It was discovered on August 7, 2000 by a team led by Michel Mayor. It is most stable if its inclination is about 65 or 115, yielding a mass of about 1.85 that of Jupiter. See also * Iota Horologii b * 79 Ceti b 79 Ceti b (also known as ''HD 16141 b'') is an extrasolar planet orbiting 79 Ceti every 75 days. Discovered along with HD 46375 b on March 29, 2000, it was the joint first known extrasolar planet to have minimum mass less than the mass of Sat ... * 94 Ceti References External links {{DEFAULTSORT:94 Ceti B Cetus (constellation) Exoplanets discovered in 2000 Exoplanets detected by radial velocity ...
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79 Ceti B
79 Ceti b (also known as ''HD 16141 b'') is an extrasolar planet orbiting 79 Ceti every 75 days. Discovered along with HD 46375 b on March 29, 2000, it was the joint first known extrasolar planet to have minimum mass less than the mass of Saturn Saturn is the sixth planet from the Sun and the second-largest in the Solar System, after Jupiter. It is a gas giant with an average radius of about nine and a half times that of Earth. It has only one-eighth the average density of Earth; h .... See also * 94 Ceti b References * External links SolStation: 79 CetiExtrasolar Planets Encyclopaedia: HD 16141 Cetus (constellation) Exoplanets discovered in 2000 Giant planets Exoplanets detected by radial velocity {{extrasolar-planet-stub ...
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6 Lyncis B
6 Lyncis b (abbreviated 6 Lyn b) is an extrasolar planet orbiting the K-type subgiant star 6 Lyncis which is approximately 182 light years away in the Lynx constellation. The planet has a minimum mass . The orbital period for this planet is 899 days, or 2.46 years. The orbital radius for this planet is 2.2 AU, periastron 1.9 AU, and apastron 2.5 AU, corresponding to the orbital eccentricity of 0.134. This planet was discovered on July 3, 2008 by Sato ''et al.'', who used Doppler spectroscopy to find variations of the line of sight motion of the star caused by the planet’s gravity during its orbit. See also * 14 Andromedae b * 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 or ... * 81 Ceti b References External links * * Lynx (constellation) Giant plane ...
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14 Andromedae B
14 Andromedae b (abbreviated 14 And b), formally named Spe , is an exoplanet approximately 249 light years away in the constellation of Andromeda. The 186-day period planet orbits about 83% the Earth- Sun distance from the giant star 14 Andromedae. It has a minimum mass 4.8 times the mass of Jupiter. The planet orbits with an eccentricity of 0.0094, which means the orbital distance over the course of its revolution varies by only 0.02 AU. Nomenclature 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 name Spe for this planet. The winning name was based on that submitted by the Thunder Bay Centre of the Royal Astronomical Society of Canada); namely 'Spes', Latin for 'hope'. (Spes was also the Roman goddess of hope.) The IAU substituted the ablative form 'Spe', w ...
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Okayama Astrophysical Observatory
The (NAOJ) is an astronomical research organisation comprising several facilities in Japan, as well as an observatory in Hawaii and Chile. It was established in 1988 as an amalgamation of three existing research organizations - the Tokyo Astronomical Observatory of the University of Tokyo, International Latitude Observatory of Mizusawa, and a part of Research Institute of Atmospherics of Nagoya University. In the 2004 reform of national research organizations, NAOJ became a division of the National Institutes of Natural Sciences. Facilities ;Mitaka Campus ( Mitaka, Tokyo. ) :The Headquarters, Astronomy Data Center, Advanced Technology Center, Public Relations Center :Solar Flare Telescope, Sunspot Telescope, TAMA 300 gravitational wave detector :Tokyo Photoelectric Meridian Circle :Historical instruments: Solar Tower Telescope, 65cm refractor dome, 20cm refractor dome ;Nobeyama Radio Observatory (Minamimaki, Nagano, ) :45m Millimeter Radio Telescope, Nobeyama Radio Pol ...
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ArXiv
arXiv (pronounced "archive"—the X represents the Greek letter chi ⟨χ⟩) is an open-access repository of electronic preprints and postprints (known as e-prints) approved for posting after moderation, but not peer review. It consists of scientific papers in the fields of mathematics, physics, astronomy, electrical engineering, computer science, quantitative biology, statistics, mathematical finance and economics, which can be accessed online. In many fields of mathematics and physics, almost all scientific papers are self-archived on the arXiv repository before publication in a peer-reviewed journal. Some publishers also grant permission for authors to archive the peer-reviewed postprint. Begun on August 14, 1991, arXiv.org passed the half-million-article milestone on October 3, 2008, and had hit a million by the end of 2014. As of April 2021, the submission rate is about 16,000 articles per month. History arXiv was made possible by the compact TeX file format ...
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Extrasolar Planet
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, initially detected in 1988, was confirmed in 2003. There are many methods of detecting exoplanets. Transit (astronomy), Transit photometry and Doppler spectroscopy have found the most, but these methods suffer from a clear observational bias favoring the detection of planets near the star; thus, 85% of the exoplanets detected are inside the tidal locking zone. In several cases, List of multiplanetary systems, multiple planets have been observed around a star. About 1 in 5 Solar analog, Sun-like starsFor the purpose of this 1 in 5 statistic, "Sun-like" means G-type star. Data for Sun-like stars was not available so this statistic is an extrapolation from data about K-type star, K-type stars. have an "Earth-sized"For the purpose of this 1 in 5 ...
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