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HD 145377 B
HD 145377 b is an extrasolar planet located approximately 180 light-years away This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile. See also * BD-17°63 b * HD 131664 * HD 143361 b * HD 147513 b * HD 153950 b * HD 20868 b * HD 43848 * HD 48265 b * HD 73267 b HD 73267 b is an extrasolar planet located approximately 164 light-years away. This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Ataca ... References External links * Exoplanets discovered in 2008 Giant planets Scorpius Exoplanets detected by radial velocity {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
La Silla Observatory
La Silla Observatory is an astronomy, astronomical observatory in Chile with three telescopes built and operated by the European Southern Observatory (ESO). Several other telescopes are located at the site and are partly maintained by ESO. The observatory is one of the largest in the Southern Hemisphere and was the first in Chile to be used by ESO. The La Silla telescopes and instruments are located 150 km northeast of La Serena, Chile, La Serena at the outskirts of the Chilean Atacama Desert, one of the driest and most remote areas of the world. Like other observatories in this geographical area, La Silla is located far from sources of light pollution and, like the Paranal Observatory, home to the Very Large Telescope, it has one of the darkest night skies on the Earth. History Following the decision in 1963 to approve Chile as the site for the ESO observatory, scouting parties were sent to various locations to assess their suitability. The site that was decided upon was ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 143361 B
HD 143361 b is an exoplanet located approximately 224 light-years away in the constellation of Norma, orbiting the 9th magnitude G-type main sequence star HD 143361. This planet has a minimum mass of 3.0 times that of Jupiter. Because the inclination was initially unknown, the true mass was not known. This planet orbits at a distance of 2.0 AU with an orbital eccentricity of 0.18. This object was detected using the radial velocity method during an astronomical survey conducted by the Magellan Planet Search Program using the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope. In 2023, the inclination and true mass of HD 143361 b were determined via astrometry Astrometry is a branch of astronomy that involves precise measurements of the positions and movements of stars and other celestial bodies. It provides the kinematics and physical origin of the Solar System and this galaxy, the Milky Way. His .... References External links * Exoplanets discov ... [...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] |
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 habitab ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 73267 B
HD 73267 b is an extrasolar planet located approximately 164 light-years away. This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile. In 2022, the inclination and true mass of HD 73267 b were measured via astrometry. See also * BD-17°63 b * HD 131664 * HD 143361 b * HD 145377 b * HD 153950 b * HD 20868 b * HD 43848 * HD 48265 b * HD 73256 b References External links * Exoplanets discovered in 2008 Giant planets Pyxis (constellation) Exoplanets detected by radial velocity Exoplanets detected by astrometry {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 48265 B
HD 48265 b is an extrasolar planet located approximately 293 light-years away in the constellation of Puppis, orbiting the 8th magnitude G-type main sequence star HD 48265. This planet has a minimum mass of 1.47 times that of Jupiter. Because the inclination is not known, the true mass is not known. This planet orbits at a distance of 1.81 AU with an orbital eccentricity of 0.08. As part of the NameExoWorlds project of the IAU, HD 48265 b has been named "Naqaỹa" ("brother") and HD 48265 "Nosaxa" ("springtime") in the Moqoit language, as voted by Argentine Argentines (mistakenly translated Argentineans in the past; in Spanish (masculine) or (feminine)) are people identified with the country of Argentina. This connection may be residential, legal, historical or cultural. For most Argentines, s ... voters in an online poll. References External links * Exoplanets discovered in 2008 Giant planets Puppis Exoplanets detected by radial velocity Exoplanets with ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 43848
HD 43848 is a 9th magnitude K-type subgiant star located approximately 123 light-years away in the constellation of Columba. The star is less massive than the Sun. On October 29, 2008, radial velocity measurements made with the MIKE echelle spectrograph on the 6.5-m Magellan II (Clay) telescope revealed the presence of a companion of at least 25 Jupiter masses orbiting the star. Initially thought to be a brown dwarf, astrometric measurements reveal that the true mass of the object is 120 Jupiter masses, implying that it is likely to be a red dwarf star. See also * BD-17°63 b * HD 131664 * HD 145377 b * HD 153950 b * HD 20868 b * HD 73267 b HD 73267 b is an extrasolar planet located approximately 164 light-years away. This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Ataca ... References K-type subgiants 043848 029804 Columba (constellation) ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 20868 B
HD 20868 b is an extrasolar planet located approximately 156 light-years away in the constellation of Fornax, orbiting the 10th magnitude K-type subgiant star HD 20868. This planet has a minimum mass of 1.99 times more than Jupiter and orbits at a distance of 0.947 AU. This planet takes 380.85 days or 12.5 months to revolve around the star with an eccentricity of 0.75, one of the most eccentric of any known extrasolar planets. At periastron, the distance is 0.237 AU and at apastron, the distance is 1.66 AU. The planet HD 20868 b is named Baiduri. The name was selected in the NameExoWorlds campaign by Malaysia, during the 100th anniversary of the IAU. Baiduri means opal in Malay language. This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO’s 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile. See also * BD-17°63 b * HD 131664 * HD 143361 b * HD 145377 b * HD 153950 b * HD 20782 b * HD 43848 * ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 153950 B
HD 153950 b, also known as Trimobe, is an extrasolar planet located approximately 162 light-years away. This planet was discovered on October 26, 2008 by Moutou ''et al.'' using the HARPS spectrograph on ESO's 3.6 meter telescope installed at La Silla Observatory in Atacama desert, Chile. The planet HD 153950 b is named Trimobe. The name was selected in the NameExoWorlds campaign by Madagascar, during the 100th anniversary of the IAU. Trimobe is a rich ogre from Malagasy tales. Characteristics Mass and orbit HD 153950 b is a Jupiter-size exoplanet. The estimated minimum mass is 2.73 times the mass of Jupiter. The planet has been found to orbit its host star every 500 days at a distance of 1.28 AU, which is approximately 28% more of the mean distance between the Sun and the Earth. HD 153950 b has a mildly elliptical orbit, given its orbital eccentricity of 0.34. Temperature The temperature of the exoplanet is likely to vary during its orbit, temperatures would likely range from ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 147513 B
HD 147513 b is an exoplanet approximately 42 light-years away in the constellation of Scorpius. It is at least 21% more massive than Jupiter. But unlike Jupiter, it orbits the star much closer, mean distance being only a third more than Earth's distance from the Sun. Its orbit is also eccentric; at periastron, it is closer to its star than Earth is from the Sun, whereas at apastron, it is further from its star than Mars Mars is the fourth planet from the Sun and the second-smallest planet in the Solar System, only being larger than Mercury (planet), Mercury. In the English language, Mars is named for the Mars (mythology), Roman god of war. Mars is a terr ... to the Sun, finding itself on the outer edge of the habitable zone. References {{extrasolar-planet-stub HD 147513 Exoplanets discovered in 2002 Giant planets Exoplanets detected by radial velocity ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 131664
HD 131664 is an 8th apparent magnitude, magnitude star in the southern constellation of Apus with an orbiting brown dwarf or stellar companion. Stellar parallax, Parallax measurements by the Gaia (spacecraft), Gaia space observatory provide an estimated distance of 172.5 light years from the Earth. The system is moving further away with a baseline heliocentric radial velocity of +35 km/s. The primary component is an ordinary G-type main-sequence star with a stellar classification of G3 V. The star is particularly metal-rich ([Fe/H] = 0.28) in comparison with the mean metallicity of the solar neighborhood. It is about 2.3 billion years old with a projected rotational velocity of 3 km/s. The star has 110% of the mass of the Sun and 116% times the Sun's radius. It is radiating 160% of the Sun's luminosity from its photosphere at an effective temperature of 5,901 K. The discovery of a brown dwarf in orbit around HD 131664 was announced on October ... [...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] |
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