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OGLE-TR-113b
OGLE-TR-113b is an extrasolar planet orbiting the star OGLE-TR-113. In 2002 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object. Since low-mass red dwarfs and brown dwarfs may mimic a planet, radial velocity measurements were necessary to calculate the mass of the body. In 2004, the object was proved to be a new transiting extrasolar planet. The planet has a mass 1.32 times that of Jupiter. Since the planet's inclination is known, the value is exact. It orbits the star (OGLE-TR-113) in an extremely close orbit, even closer than the famous planets 51 Pegasi b and HD 209458 b. The planet races around the star every 1.43 days. The radius of the planet is only 9% larger than Jupiter's, despite the heating effect by the star. Planets of its kind are sometimes called "super-hot Jupiters". See also * OGLE-TR-132b *List of extrasolar planets * OGLE-TR-10b * OGLE-TR-111b * OGLE-TR-56b * ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-TR-113
OGLE-TR-113 is a dim, distant magnitude 16 binary star in the star fields of the constellation Carina. Because of its distance of about 1170 light years, and location in a crowded field it was not notable in any way. Its apparent brightness changes when one of its planets transits, so the star has been given the variable star designation V752 Carinae. Spectral type of the star is type K dwarf star, slightly cooler and less luminous than the Sun. Planetary system However, in 2002 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object. Since low-mass red dwarfs and brown dwarfs may mimic a planet radial velocity measurements were necessary to calculate the mass of the body. In 2004 the object was proved to be a new transiting extrasolar planet, OGLE-TR-113b. See also * OGLE-TR-132 * Optical Gravitational Lensing Experiment * List of extrasolar planets Thes ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE2-TR-L9b
OGLE2-TR-L9b is an extrasolar planet discovered by three undergraduate students from Leiden University, Netherlands. The planet is about 4.5 times as massive as Jupiter and is the first discovered planet orbiting a fast-rotating hot star. Initially discovered while testing a method for investigating light fluctuations in the OGLE database, the planet's existence was later confirmed by follow-up observations from the ESO's Very Large Telescope in Chile. See also * Optical Gravitational Lensing Experiment OGLE * OGLE-TR-113b * OGLE-TR-10b * OGLE-TR-111b * OGLE-TR-56b OGLE-TR-56b is an extrasolar planet located approximately 1500 parsecs away in the constellation of Sagittarius, orbiting the star OGLE-TR-56. This planet was the first known exoplanet to be discovered with the transit method. The object was d ... References External links * Students Discover Unique Planet* Exoplanets discovered in 2008 Giant planets Hot Jupiters Transiting exoplanets Cari ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-TR-56b
OGLE-TR-56b is an extrasolar planet located approximately 1500 parsecs away in the constellation of Sagittarius, orbiting the star OGLE-TR-56. This planet was the first known exoplanet to be discovered with the transit method. The object was discovered by the OGLE project, announced on July 5, 2002 and confirmed on January 4, 2003 by the Doppler technique. The period of this confirmed planet was the shortest until the confirmed discovery of WASP-12b on April 1, 2008. The short period and proximity of the OGLE-TR-56 b to its host mean it belongs to a class of objects known as hot Jupiters. The planet is thought to be only 4 stellar radii from its star, and hot enough to have iron rain. See also * Optical Gravitational Lensing Experiment (OGLE) * OGLE-TR-113b * OGLE-TR-10b * OGLE-TR-111b * OGLE2-TR-L9b OGLE2-TR-L9b is an extrasolar planet discovered by three undergraduate students from Leiden University, Netherlands. The planet is about 4.5 times as massive as Jupi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-TR-111b
OGLE-TR-111b is an extrasolar planet approximately 5,000 light-years away in the constellation of Carina (the Keel). The planet is currently the only confirmed planet orbiting the star OGLE-TR-111 (though a possible second planet is plausible). In 2002 the Optical Gravitational Lensing Experiment (OGLE) survey detected that the light from the star periodically dimmed very slightly every 4 days, indicating a planet-sized body transiting the star. But since the mass of the object had not been measured, it was not clear that it was a true planet, low-mass red dwarf or something else. In 2004 radial velocity measurements showed unambiguously that the transiting body is indeed a planet. The planet is probably very similar to the other hot Jupiters orbiting nearby stars. Its mass is about half that of Jupiter and it orbits the star at a distance less than 1/20th that of Earth from the Sun. OGLE-TR-111b has similar mass and orbital distance as the first transiting planet, HD 20945 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-TR-132b
OGLE-TR-132b is an extrasolar planet orbiting the star OGLE-TR-132. In 2003 the Optical Gravitational Lensing Experiment (OGLE) detected periodic dimming in the star's light curve indicating a transiting, planetary-sized object. Since low-mass red dwarfs and brown dwarfs may mimic a planet radial velocity measurements were necessary to calculate the mass of the body. In 2004 the object was proved to be a new transiting extrasolar planet. The planet has a mass 1.14 times that of Jupiter. Since the planet's inclination is known, this represents the best measured true mass of the planet, rather than simply the minimum mass as is the case when the inclination is unknown. It orbits the star (OGLE-TR-132) in an extremely close orbit, even closer than the famous planets 51 Pegasi b and HD 209458 b. The planet races around the star every 1 day 16.6 hours. The radius of the planet is only 18% larger than Jupiter's, despite the heating effect by the star. Planets of its kind are ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Osiris (planet)
HD 209458 b, which is also nicknamed Osiris after the Egyptian god, is an exoplanet that orbits the Solar twin, solar analog HD 209458 in the constellation Pegasus (constellation), Pegasus, some from the Solar System. The radius of the planet's orbit is , or one-eighth the radius of Mercury (planet), Mercury's orbit (). This small radius results in a year that is 3.5 Earth-days long and an estimated surface temperature of about . Its mass is 220 times that of Earth (0.69 Jupiter masses) and its volume is some 2.5 times greater than that of Jupiter. The high mass and volume of HD 209458 b indicate that it is a gas giant. HD 209458 b represents a number of milestones in extraplanetary research. It was the first of many categories: * a Astronomical transit, transiting extrasolar planet * The first planet detected through more than one method * an extrasolar planet known to have an atmosphere * an extrasolar planet observed to have an evaporating hydrogen atmosphere * an extrasolar p ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Exoplanets Discovered In 2002
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.F ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Hot Jupiters
Hot Jupiters (sometimes called hot Saturns) are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods (). The close proximity to their stars and high surface-atmosphere temperatures resulted in their informal name "hot Jupiters". Hot Jupiters are the easiest extrasolar planets to detect via the radial-velocity method, because the oscillations they induce in their parent stars' motion are relatively large and rapid compared to those of other known types of planets. One of the best-known hot Jupiters is . Discovered in 1995, it was the first extrasolar planet found orbiting a Sun-like star. has an orbital period of about 4 days. General characteristics Though there is diversity among hot Jupiters, they do share some common properties. * Their defining characteristics are their large masses and short orbital periods, spanning 0.36–11.8 Jupiter masses and 1.3–111 Earth days. The mass ca ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
OGLE-TR-10b
OGLE-TR-10b is an extrasolar planet orbiting the star OGLE-TR-10. The planet was first detected by the Optical Gravitational Lensing Experiment ( OGLE) survey in 2002. The star, OGLE-TR-10, was seen dimming by a tiny amount every three days. The transit lightcurve resembles that of HD 209458 b, the first transiting extrasolar planet. However, the mass of the object had to be measured by the radial velocity method because other objects like red dwarfs and brown dwarfs can mimic the planetary transit. In late 2004 it was confirmed as the fifth planetary discovery by OGLE. The planet is a typical "hot Jupiter", a planet with a mass half that of Jupiter and orbital distance only 1/24 that of Earth from the Sun. One revolution around the star takes a little over three days to complete. The planet is slightly larger than Jupiter, probably due to the heat from the star. OGLE-TR-10 was identified as a promising candidate by the OGLE team during their 2001 campaign in three fields toward ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Extrasolar Planets
These are lists of exoplanets. Most of these were discovered by the Kepler space telescope. There are an additional 2,054 potential exoplanets from Kepler's first mission yet to be confirmed, as well as 978 from its " Second Light" mission and 4,081 from the Transiting Exoplanet Survey Satellite (TESS) mission. For yearly lists on physical, orbital and other properties, as well as on discovery circumstances and other aspects, ''see ''. Nomenclature Methods of detection Specific exoplanet lists Lists of exoplanets *List of directly imaged exoplanets * List of exoplanets discovered before 2000 () * List of exoplanets discovered between 2000–2009 () * List of exoplanets discovered in 2010 () * List of exoplanets discovered in 2011 () *List of exoplanets discovered in 2012 () * List of exoplanets discovered in 2013 () * List of exoplanets discovered in 2014 () *List of exoplanets discovered in 2015 () *List of exoplanets discovered in 2016 () *List of exoplanets discov ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Hot Jupiter
Hot Jupiters (sometimes called hot Saturns) are a class of gas giant exoplanets that are inferred to be physically similar to Jupiter but that have very short orbital periods (). The close proximity to their stars and high surface-atmosphere temperatures resulted in their informal name "hot Jupiters". Hot Jupiters are the easiest extrasolar planets to detect via the radial-velocity method, because the oscillations they induce in their parent stars' motion are relatively large and rapid compared to those of other known types of planets. One of the best-known hot Jupiters is . Discovered in 1995, it was the first extrasolar planet found orbiting a Sun-like star. has an orbital period of about 4 days. General characteristics Though there is diversity among hot Jupiters, they do share some common properties. * Their defining characteristics are their large masses and short orbital periods, spanning 0.36–11.8 Jupiter masses and 1.3–111 Earth days. The mass ca ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
