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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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Royal Astronomical Society Of Canada
Royal may refer to: People * Royal (name), a list of people with either the surname or given name * A member of a royal family Places United States * Royal, Arkansas, an unincorporated community * Royal, Illinois, a village * Royal, Iowa, a city * Royal, Missouri, an unincorporated community * Royal, Nebraska, a village * Royal, Franklin County, North Carolina, an unincorporated area * Royal, Utah, a ghost town * Royal, West Virginia, an unincorporated community * Royal Gorge, on the Arkansas River in Colorado * Royal Township (other) Elsewhere * Mount Royal, a hill in Montreal, Canada * Royal Canal, Dublin, Ireland * Royal National Park, New South Wales, Australia Arts, entertainment, and media * ''Royal'' (Jesse Royal album), a 2021 reggae album * ''The Royal'', a British medical drama television series * ''The Royal Magazine'', a monthly British literary magazine published between 1898 and 1939 * ''Royal'' (Indian magazine), a men's lifestyle bimonthly * Royal ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Exoplanets Discovered In 2008
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 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, multiple planets have been observed around a star. About 1 in 5 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 stars. have an "Earth-sized"For the purpose of this 1 in 5 statistic, Earth-sized means 1–2 Earth radii. planet in the habitable zone. ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ablative (Latin)
In Latin grammar, the ablative case () is one of the six cases of nouns. Traditionally, it is the sixth case (). It has forms and functions derived from the Proto-Indo-European ablative, instrumental, and locative. It expresses concepts similar to those of the English prepositions ''from''; ''with'', ''by''; and ''in'', ''at''. It is sometimes called the adverbial case, since phrases in the ablative can be translated as adverbs: , "with incredible speed", or "very quickly". Uses Ablative proper Some uses of the ablative descend from the Proto-Indo-European ablative case. * Ablative of separation implies that some person or thing is separated from another. No active movement from one location to the next occurs; furthermore, ablatives of separation sometimes lack a preposition, particularly with certain verbs like ''careō'' or ''līberō''. For example, ''Cicerō hostēs ab urbe prohibuit'', "Cicero kept the enemy away from the city"; ''eōs timōre līberāvit'', "he freed the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Spes
In ancient Roman religion, Spes (pronounced ) was the goddess of hope. Multiple temples to Spes are known, and inscriptions indicate that she received private devotion as well as state cult. Republican Hope During the Republic, a temple to "ancient Hope" ''(Spes vetus)'' was supposed to have been located near the Praenestine Gate. It was associated with events that occurred in the 5th century BC, but its existence as anything except perhaps a private shrine has been doubted. A well-documented temple of Spes was built by Aulus Atilius Calatinus along with Fides, as the result of vows ''(vota)'' made to these goddesses during the First Punic War. At Capua in 110 BC, a temple was built to the triad of Spes, Fides, and Fortuna. Imperial Hope Spes was one of the divine personifications in the Imperial cult of the Virtues. Spes Augusta was Hope associated with the capacity of the emperor as ''Augustus'' to ensure blessed conditions. Like Salus ("Salvation, Security"), Ops ("Abunda ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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