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Kepler-1704b
Kepler-1704b is a super-Jupiter on a highly eccentric orbit around the star Kepler-1704. It has a mass of 4.51 . The planet's distance from its star varies from 0.16 to 3.9 Astronomical unit, AU. It is a failed hot Jupiter, having been scattered from its birth orbit to orbit with a periastron just above the tidal circularization distance. Characteristics Kepler-1704b is much more massive than Jupiter, at 4.51 M''J.'' The high planetary mass makes Kepler-1704b a super-Jupiter. Kepler-1704b goes on a highly eccentric 2.7 year-long (988.88 days) orbit around its star as well as Methods of detecting exoplanets, transiting. The extreme eccentricity yields a temperature difference of up to 700 K. Star The star, Kepler-1704, is a G2, 5745-kelvin star from Earth and the sun. It has a mass of , a radius of , and a luminosity of . The high radius for the star's mass hints that Kepler-1704 is not a Main sequence, main-sequence star. See also *Gas giant *List of planet types *Kepler-419b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gas Giant
A gas giant is a giant planet composed mainly of hydrogen and helium. Jupiter and Saturn are the gas giants of the Solar System. The term "gas giant" was originally synonymous with "giant planet". However, in the 1990s, it became known that Uranus and Neptune are a distinct class of giant planets composed mainly of heavier volatile substances (referred to as "Volatile (astrogeology)#Planetary science, ices"). For this reason, Uranus and Neptune are often classified in the separate category of ice giants. Jupiter and Saturn consist mostly of hydrogen and helium, with heavier elements making up between 3 and 13 percent of their mass.The Interior of Jupiter, Guillot et al., in ''Jupiter: The Planet, Satellites and Magnetosphere'', Bagenal et al., editors, Cambridge University Press, 2004 They are thought to have an outer layer of compressed molecular hydrogen surrounding a layer of liquid metallic hydrogen, with a molten rocky core inside. The outermost portion of their hydrogen atmo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Super-Jupiter
A super-Jupiter is a gas giant exoplanet that is more massive than the planet Jupiter. For example, substellar companion, companions at the planet–brown dwarf borderline have been called super-Jupiters, such as around the star Kappa Andromedae. Makeup By 2011 there were 180 known super-Jupiters, some Hot Jupiter, hot, some cold. Even though they are more massive than Jupiter, they remain about the same size as Jupiter up to 80 Jupiter masses. This means that their surface gravity and density go up proportionally to their mass. The increased mass Gravitational compression, compresses the planet due to gravity, thus keeping it from being larger. In comparison, planets somewhat lighter than Jupiter can be larger, so-called "puffy planets" (gas giants with a large diameter but low density). An example of this may be the exoplanet HAT-P-1b with about half the mass of Jupiter but about 1.38 times larger diameter. CoRoT-3b CoRoT-3b, with a mass around 22 Jupiter masses, is predict ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eccentric Orbit
In astrodynamics, the orbital eccentricity of an astronomical object is a dimensionless quantity, dimensionless parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabola, parabolic escape orbit (or capture orbit), and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a klemperer rosette, rosette orbit through the Galaxy. Definition In a two-body problem with inverse-square-law force, every orbit is a Kepler orbit. The eccentricity (mathematics), eccentricity of this Kepler orbit is a non-negative number that defines its shape. The eccentricity may take the following values: * Circular orbit: * Elliptic orbit: * Parabolic trajectory: * Hyperbolic t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astronomical Unit
The astronomical unit (symbol: au or AU) is a unit of length defined to be exactly equal to . Historically, the astronomical unit was conceived as the average Earth-Sun distance (the average of Earth's aphelion and perihelion), before its modern redefinition in 2012. The astronomical unit is used primarily for measuring distances within the Solar System or around other stars. It is also a fundamental component in the definition of another unit of astronomical length, the parsec. One au is approximately equivalent to 499 light-seconds. History of symbol usage A variety of unit symbols and abbreviations have been in use for the astronomical unit. In a 1976 resolution, the International Astronomical Union (IAU) had used the symbol ''A'' to denote a length equal to the astronomical unit. In the astronomical literature, the symbol AU is common. In 2006, the International Bureau of Weights and Measures (BIPM) had recommended ua as the symbol for the unit, from the French ... [...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 (i.e. Jupiter analogue, Jupiter analogues) 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, 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 four 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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Methods Of Detecting Exoplanets
Methods of detecting exoplanets usually rely on indirect strategies – that is, they do not directly Astrophotography, image the planet but deduce its existence from another signal. Any planet is an extremely faint light source compared to its parent star. For example, a star like the Sun is about a billion times as bright as the reflected light from any of the planets orbiting it. In addition to the intrinsic difficulty of detecting such a faint light source, the Glare (vision), glare from the parent star washes it out. For those reasons, very few of the exoplanets reported have been detected directly, with even fewer being resolved from their host star. Established detection methods The following methods have proven successful at least once for discovering a new planet or detecting an already discovered planet: Radial velocity A star with a planet will move in its own small orbit in response to the planet's gravity. This leads to variations in the speed with which the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Main Sequence
In astronomy, the main sequence is a classification of stars which appear on plots of stellar color index, color versus absolute magnitude, brightness as a continuous and distinctive band. Stars on this band are known as main-sequence stars or dwarf stars, and positions of stars on and off the band are believed to indicate their physical properties, as well as their progress through several types of star life-cycles. These are the most numerous true stars in the universe and include the Sun. Color-magnitude plots are known as Hertzsprung–Russell diagrams after Ejnar Hertzsprung and Henry Norris Russell. After condensation and ignition of a star, it generates thermal energy in its dense stellar core, core region through nuclear fusion of hydrogen into helium. During this stage of the star's lifetime, it is located on the main sequence at a position determined primarily by its mass but also based on its chemical composition and age. The cores of main-sequence stars are in hydros ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Planet Types
The following is a list of planet types by their mass, orbit, physical and chemical composition, or by another classification. By mass regime By orbital regime By composition Other types See also * * Dwarf planet * Minor planet * * Stellar classification * Substellar object * Sudarsky's gas giant classification Notes References External links Periodic Table of ExoplanetsaPlanetary Habitability Laboratory University of Puerto Rico at Arecibo A Thermal Planetary Habitability Classification for ExoplanetsA Mass Classification for both Solar and Extrasolar Planetsat NASA The National Aeronautics and Space Administration (NASA ) is an independent agencies of the United States government, independent agency of the federal government of the United States, US federal government responsible for the United States ... Stern and Levison, "Regarding the criteria for planethood and proposed planetary classification schemes," Highlights of Astronomy 12 ( ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kepler-419b
Kepler-419b (also known by its Kepler Object of Interest designation ''KOI-1474.01'') is a hot Jupiter exoplanet orbiting the star Kepler-419, the outermost of two such planets discovered by NASA's Kepler spacecraft. It is located about 3,400 light-years (1040 parsecs from Earth in the constellation Cygnus. Characteristics Mass, radius and temperature Kepler-419b is a hot Jupiter, an exoplanet that has a radius and mass near that of the planet Jupiter, but with a much higher temperature. It has a temperature of .Kepler 419 hpcf.upr.edu It has a mass of 2.5 and a radius of 0.96 . Host star The planet orbits an ( F-type) |
HD 80606 B
HD 80606 b (also Struve 1341 Bb or HIP 45982 b) is an eccentric Jupiter, eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Michel Mayor and Didier Queloz. With a mass 4 times that of Jupiter, it is a gas giant. Because the planet Astronomical transit, transits the host star its radius can be determined using the Transit method#Transit photometry, transit method, and was found to be about the same as Jupiter's. Its density is slightly less than Earth's. It has an extremely eccentric orbit like a comet, with its orbit taking it very close to its star and then back out very far away from it every 111 days. Discovery The variable radial velocity of HD 80606 was first noticed in 1999 from observations with the 10-m Keck 1 telescope at the W. M. Keck Observatory in Hawaii by the G-Dwarf Planet Search, a survey of nearly 1000 nearby G dwarfs to identify extrasolar pl ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HR 5183 B
HR 5183 b is an exoplanet located 102.7 light year A light-year, alternatively spelled light year (ly or lyr), is a unit of length used to express astronomical distance, astronomical distances and is equal to exactly , which is approximately 9.46 trillion km or 5.88 trillion mi. As defined by t ...s away in the constellation of Virgo (constellation), Virgo orbiting the star HR 5183. It has a mass of . It has a highly Orbital eccentricity, eccentric (e≃0.87) orbit which takes it from within the orbit of Jupiter to beyond the orbit of Neptune (2.87 to 41.8Astronomical unit, AU) which classifies it as an eccentric Jupiter and it has been nicknamed the "whiplash planet". It was discovered in 2019 based on two decades of Doppler spectroscopy, radial velocity observations. In 2021, astrometry, astrometric observations revealed that HR 5183 b has a nearly edge-on orbital inclination, and thus its true mass is close to its minimum mass. See also * Eccentric Jupiter *HD 80606 b * ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 20782 B
HD 20782 b is an extrasolar planet located approximately 117 light-years away in the constellation of Fornax, orbiting the star HD 20782. This planet orbits in the most eccentric orbit known (as of November 2012), with a semi-major axis of 1.36 AU, and eccentricity e=0.97+/-0.01. As a result, it also has one of the most extreme temperature swings. See also * HD 80606 b HD 80606 b (also Struve 1341 Bb or HIP 45982 b) is an eccentric Jupiter, eccentric hot Jupiter 217 light-years from the Sun in the constellation of Ursa Major. HD 80606 b was discovered orbiting the star HD 80606 in April 2001 by a team led by Mi ... References External links * Fornax Exoplanets discovered in 2006 Giant planets Exoplanets detected by radial velocity {{extrasolar-planet-stub de:HD 20782 b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
