HD 118203 b [SEP] site of astronomical discovery
HD 118203 b


HD 118203 b is a jovian planet that takes only 6.13 days or 147 hours to orbit the parent star at a distance of 0.07 astronomical units. It has minimum mass of 2.14 times that of Jupiter but the true mass is not known since inclination is not known. This hot Jupiter is unusual since it has relatively high eccentricity of 0.31. HD 118203 b was discovered in August 2005 in Haute-Provence Observatory in France by Da Silva who used the doppler spectroscopy to look for shifts in the star's spectrum caused by the
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HD 17092 b


HD 17092 b is an extrasolar planet located approximately 750 light years away in the constellation Perseus, orbiting the giant star HD 17092. In 2007 discovery of an extrasolar planet orbiting HD 17092 was announced by a team led by Andrzej Niedzielski of Polish Nicolaus Copernicus University and including astronomers from Penn State, the Spitzer Science Center, the Jet Propulsion Laboratory, and the University of Texas. The discovery was made using the Hobby-Eberly Telescope. The planet, designated as HD 17092 b, has a minimum mass of 4.6 Jupiter masses
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HD 154672 b


MIKE) at Las Campanas Observatory in Chile since 2004. Based on these observations, the stars HD 154672 and HD 205739 were among those flagged as potential planetary host stars. The two stars were identified originally as having short-orbit hot Jupiter planets, but 3.5 years of additional observations revealed that the planetary candidates' orbits were far longer than initially anticipated. HD 154672 b's discovery was reported in the "Astronomical Journal" by the American Astronomical Society, appearing in the journal on October 7, 2008 alongside the planet HD
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HD 154672


Telescopes at Chile's Las Campanas Observatory. Use of the Magellan Clay telescope's Magellan Inamori Kyocera Echelle spectrograph (MIKE) helped collect sixteen radial velocity measurements for HD 154672; a team of American astronomers and one from the Vatican City used these measurements to confirm the existence of planet HD 154672 b and to determine its mass. The discovery of HD 154672's planet was reported in the "Astronomical Journal" on October 7, 2008 along with a planet in the orbit of HD 205739. HD 154672 is a sunlike G-
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Mikko Tuomi


Mikko Tuomi is a Finnish astronomer from the University of Hertfordshire, most known for his contributions to the discovery of a number of exoplanets, among them the Proxima Centauri b which orbits the closest star to the Sun. Mikko Tuomi was the first to find indications of the existence of Proxima Centauri b in archival observation data. Other exoplanets to whose discovery or study Tuomi has contributed include HD 40307, HD 154857 c, Kapteyn c, Gliese 682 c, HD 154857, Gliese 221, Gliese 581 g and the planetary system orbiting
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HD 102272 b


HD 102272 b is an extrasolar planet approximately 1,200 light-years away in the constellation of Leo. The planet was discovered orbiting the K-type giant star HD 102272 in 2008. The planet was discovered by the radial velocity method, using the Hobby-Eberly Telescope. Another planet, HD 102272 c, was also discovered orbiting the same star. The discovery was announced in June 2008. HD 102272 b orbits at an average of 0.614 astronomical units away from its star, with a mass at least 5.9 ± 0.2 times
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HD 149026 b


HD 149026 b, formally named Smertrios , is an extrasolar planet approximately 250 light-years from the Sun in the constellation of Hercules. The 2.8766-day period planet orbits the yellow subgiant star HD 149026 at a distance of 0.042 AU and is notable first as a transiting planet, and second for a small measured radius (relative to mass and incoming heat) that suggests an exceptionally large planetary core. Following its discovery in 2005 the planet was designated HD 149026 b. In July 2014 the International Astronomical Union launched a process for giving proper
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HD 149026


HD 149026, also named Ogma , is a yellow subgiant star approximately 250 light-years from the Sun in the constellation of Hercules. An extrasolar planet (designated HD 149026 b, later named Smertrios) is believed to orbit the star. HD 149026 in the star's identifier in the Henry Draper Catalog. Following its discovery in 2005 the planet was designated HD 149026 b. In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting
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HD 104985


HD 104985, also named Tonatiuh , is a helium-fusing yellow giant star located 97 parsecs (317 lys) from the Sun in the constellation of Camelopardalis. An extrasolar planet (designated HD 104985 b, later named Meztli ) is believed to orbit the star. HD 104985 is the star's entry in the Henry Draper Catalogue. Following its discovery in 2003 the planet was designated HD 104985 b. In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process
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HD 104985 b


HD 104985 b, also named Meztli , is an extrasolar planet approximately 97 parsecs (317 lys) from the SunThe 198-day period planet orbits the yellow giant star HD 104985 (Tonatiuh) at a distance of 0.78 AU. With a mass 6/ times Jupiter it is a gas giant. Following its discovery in 2003 the planet was designated HD 104985 b. In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names.
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HD 38801 b


HD 38801 b is an extrasolar, gas giant planet located in the constellation of Orion whose discovery was announced in 2009 and was made using the radial velocity method. The object, with a mass roughly 12 times that of Jupiter, is located 324 light years (99.4 parsecs) from Earth orbiting 1.65 astronomical units from its G-type star, HD 38801. HD 38801 b, besides being the only planet in its system also lies within the inner habitable zone and takes around 1.9 years, or 693.5 days to complete a
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HD 189733 b


atmospheres on three exoplanets (HD 189733b, HD 209458b, WASP-12b) orbiting Sun-like stars. On October 6, 2005, a team of astronomers announced the discovery of transiting planet HD 189733 b. The planet was then detected using Doppler spectroscopy. Real-time radial velocity measurements detected the Rossiter–McLaughlin effect caused by the planet passing in front of its star before photometric measurements confirmed that the planet was transiting. In 2006, a team led by Drake Deming announced a detection of strong infrared thermal emission from the transiting exoplanet
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HD 16175 b


HD 16175 b is an extrasolar planet located approximately 195.6 light-years away in the constellation of Andromeda, orbiting the star HD 16175. This planet masses 4.8 times that of Jupiter. However, the mass is only a minimum since the inclination of the orbit is not known. This planet orbits at about 2.2 astronomical units, taking 2.73 years to revolve around the star. The orbit of the planet is highly noncircular with an eccentricity at 0.64. The discovery was made using radial velocity measurements taken between November 2004 and March 2009
17565000
HD 131399


B and C are located very close to each other, and the two orbit each other. In turn, the B-C pair orbits the central star A at a distance of 349 astronomical units (au). This orbit takes about 3,600 years to complete, and it has an eccentricity of about 0.13 The entire system is about 21.9 million years old. The discovery of a massive planet, named HD 131399 Ab, was announced in a paper published in the journal "Science". The object was imaged using the
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HD 156668


1993, HD 156668 was observed at least twice and was featured at the 6th annual catalog of the Tokyo Photoelectric Meridian Circle (PMC) where it is one of 6649 stars observed. Andrew Howard announced the discovery of a Super-Earth in orbit around HD 156668. This planet is designated HD 156668 b. The announcement was made at the 215th American Astronomical Society meeting on January 4 to 7, 2010 in Washington D.C.. The planet orbits its star in only 4.6 days with a distance approximately 0.05 AU away from the parent star
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HD 154672 b


HD 154672 b is an extrasolar planet located approximately 210 light-years away==Discovery== Astronomers hoped to implement a survey called the N2K Consortium, a collaboration which uses Doppler spectroscopy to find radial velocity measurements of stars that hadn't been previously surveyed. The project searched particularly for gas giants with short orbits around metal-rich stars to find how the metallicity of the star and the mass of the planet are related. Radial velocity observations had been taken by the N2K program using the Magellan Telescopes' Magellan Inamori Kyocera Echelle spectrograph (
16181720
HD 149382


The effective temperature of the star's outer envelope is about 35,500 K, giving it the characteristic blue-white hue of a B-type star. HD 149382 has a visual companion located at an angular separation of 1 arcsecond. In 2009, a substellar companion, perhaps even a superjovian planet, was announced orbiting the star. This candidate object was estimated to have nearly half the mass of the Sun. In 2011, this discovery was thrown into doubt when an independent team of astronomers were unable to confirm the detection.
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Pi Mensae b


Pi Mensae b (π Men b, π Mensae b), also known as HD 39091 b, is an extrasolar planet approximately 59 light-years away in the constellation of Mensa. The planet was announced orbiting the yellow main-sequence star Pi Mensae in October 2001. On October 15, 2001, a team of astronomers including Jones, Butler, Tinney, Marcy, Penny, McCarthy, Carter, and Pourbaix announced the discovery of one of the most massive extrasolar planets that have yet been observed. It was discovered
20826334
HD 177830


have two extrasolar planets orbiting around it. The secondary star is a Red dwarf star orbiting at a distance of 100 to 200 AU with a likely period of roughly 800 years. On November 1, 1999, the discovery of a planet HD 177830 b was announced by the California and Carnegie Planet Search team using the very successful radial velocity method and an analysis on data released by the team performed by amateur astronomer Peter Jalowiczor along with two other planets. This planet is nearly 50% more massive than Jupiter () and takes
2270427
Aquarius (constellation)


and respectively) is large enough to make this discrepancy statistically insignificant. HD 215152 c also orbits further from the star than HD 215152 b, 0.0852 AU compared to 0.0652. On 23 February 2017, NASA announced that ultracool dwarf star TRAPPIST-1 in Aquarius has seven Earth-like rocky planets. Of these, three are in the system's habitable zone, and may contain water. The discovery of the TRAPPIST-1 system is seen by astronomers as a significant step toward finding life beyond Earth. Because of its position away from the galactic
218201
HD 24040 b


HD 24040 b is a long-period exoplanet taking approximately 3500 days to orbit at 4.6 astronomical units in an almost circular orbit. It has a minimum mass 4 times that of Jupiter. HD 24040b was discovered in 2006 based on observations made at the W. M. Keck Observatory in Hawaii. However, because the observations covered less than one complete orbit there were only weak constraints on the period and mass. The first reliable orbit for HD 24040b was obtained by astronomers at Haute-Provence Observatory in 2012 who combined the keck measurements
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HD 205739 b


HD 205739 b is an extrasolar planet located approximately 350 light-years away==Discovery== HD 205739's designation is from the Henry Draper catalogue. The star was also observed by "Hipparcos", which released its catalogue in 1997. The observations that led to the discovery of the planet HD 205739 b started when the N2K Consortium started an extended search for planets around 300 stars not usually targeted by Doppler spectroscopy surveys. In the case of HD 205739, the star was observed using the Magellan Telescopes at Las Campanas Observatory in Chile.
16181745
HD 8574 b


of a sunlike star. By 2003, the discovery of six new planets, including HD 8574 b, was announced, bringing ELODIE's planet discovery count to eighteen. HD 8574, one of the target stars of ELODIE, had been previously catalogued by the European Space Agency with the release of the "Hipparcos" catalogue in 1997. Most of HD 8574's characteristics were extracted from this catalogue for use in searching for a planet around HD 8574. The spectrum was then analyzed to see if HD 8574 were active, a
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HD 189733


it is listed in the General Catalogue of Variable Stars as a BY Draconis variable with the variable star designation "V452 Vul". Discovered in 2006 by the infrared 2MASS astronomical survey, 2MASS J20004297+2242342 or "HD 189733 B" is a dim red dwarf star of spectral type M. The companion was observed at a separation of 216 astronomical units away from the primary star. Orbiting in a clockwise orbit (which is nearly perpendicular to the orbital plane of transiting planet HD 189733 b), the orbital period is estimated around
2863813
HD 102956 b


HD 102956 b is an extrasolar planet discovered in 2010 by a team of American astronomers led by John Johnson using Doppler spectroscopy and the Keck Observatory in Hawaii. HD 102956 b is in the orbit of host star HD 102956. The planet is at most the mass of Jupiter, orbiting every 6.5 days at a distance of 12 million km. HD 202956 b has a very circular orbit. The system is roughly 411 light years from us. In June 2019 this planet was announced as part of the NameExoWorlds project where it was
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HD 8574 b


HD 8574 b is an extrasolar planet discovered in 2001 by a team of European astronomers using Doppler spectroscopy as part of the ELODIE Planet Search Survey, and was published in a paper with five other planets. HD 8574 b is in the orbit of host star HD 8574. The planet is at most two times the mass of Jupiter, orbiting every 227 days at three quarters of the distance between the Earth and Sun. HD 8574 b has a very elliptical orbit, far more than that of Jupiter. The ELODIE Planet Search
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HD 37605 b


HD 37605 b is an extrasolar planet that has nearly three times more mass than Jupiter. It orbits close to the star, taking 54 days to revolve around the parent star HD 37605. Its orbit is highly eccentric, around 74%. Distance from HD 37605 ranges from 0.069 to 0.453 astronomical units. It is the first planet found by Hobby-Eberly Telescope (HET) in July 2004. In a simulation, HD 37605 b's orbit "sweeps clean" most test particles within 0.5 AU; leaving only asteroids "
17974671
55th Air Defense Artillery Regiment


December 1941; a second detachment helped form the 804th CA (HD) Btry (Sep). Btry F at Sand Is. was designated the 807th CA (HD) Btry (Sep), while a second detachment helped organize the 715th CA (HD) Btry (Sep) 10-21-42. During World War II, various changes were made in the makeup of the 55th CA. The 55th CA (155 mm Gun) Regt was reorganized and HHB reconstituted and activated; 1st, 2nd, and 3rd
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HD 11964 b


HD 11964 b is an extrasolar planet, a gas giant like Jupiter approximately 110 light-years away in the constellation of Cetus. The planet orbits the yellow subgiant star HD 11964 in a nearly-circular orbit, taking over 5 years to complete a revolution around the star at a distance of 3.34 astronomical units. The planet was discovered in 2005 and published as part of the Catalog of Nearby Exoplanets under the designation HD 11964 b. However, since that time there has been confusion as to the designations of the planets in the
4655105
HD 209458 b


HD 209458 b and two other exoplanets (HD 189733 b and WASP-12b) orbiting Sun-like stars. Spectroscopic studies first revealed the presence of a planet around HD 209458 on November 5, 1999. Astronomers had made careful photometric measurements of several stars known to be orbited by planets, in the hope that they might observe a dip in brightness caused by the transit of the planet across the star's face. This would require the planet's orbit to be inclined such that it would pass between the Earth and the star,
7889738
HD 106906 b


%. Observation of star began in 2005, utilizing the Magellan Telescopes at the Las Campanas Observatory in the Atacama Desert of Chile, some eight years before the companion was discovered. The initial interest in was directed largely to the debris disk surrounding the star, a pre-main-sequence member of Lower Centaurus Crux. On December 4, 2013, University of Arizona graduate student Vanessa Bailey, leader of an international team of astronomers, detailed the discovery of with a paper first published as a preprint on the "arXiv"
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HD 106906 b


and later as a refereed article in "The Astrophysical Journal Letters". The discovery team and astronomers worldwide were puzzled by extreme separation from its host star, because it is not considered possible that a star's protoplanetary disk could be extensive enough to permit formation of gas giants at such a distance. To account for the separation, it is theorized that the companion formed independently from its star as part of a binary system. This proposal is somewhat problematic in that the mass ratio of ~140:1 is not in the range expected from
15791557
HD 219077


-orbiting planet was deduced through radial velocity variations. This discovery was published in November of the same year. The estimated mass of the planet is at least ten times that of Jupiter. The discoverers noted that HD 219077 b is among the "three most eccentric planets with a period larger than 5 years" – along with HD 98649 b and HD 166724 b, also found with CORALIE. The reason for this eccentricity is unknown. They submitted HD 219077 b as a candidate for direct imaging, once it gets out to
13566783
HD 69830


, a team of astronomers using the European Southern Observatory's (ESO) HARPS spectrograph on the 3.6-metre La Silla telescope in the Atacama desert, Chile, announced the discovery of three extrasolar planets orbiting the star. With minimum masses between 10 and 18 times that of the Earth, all three planets are presumed to be similar to the planets Neptune or Uranus. , no planet with more than half the mass of Jupiter had been detected within three astronomical units of HD 69830. The star rotates at an inclination of 13 degrees relative
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HD 189733 b


HD 189733 b is an extrasolar planet approximately 63 light-years away from the Solar System in the constellation of Vulpecula. The planet was discovered orbiting the star HD 189733 A on October 5, 2005, when astronomers in France observed the planet transiting across the face of the star. With a mass 13% higher than that of Jupiter, HD 189733 b orbits its host star once every 2.2 days at an orbital speed of , making it a hot Jupiter with poor prospects for extraterrestrial life. Being the closest transiting hot Jupiter
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HD 154672 b


205739 b. The two planets were the first to be discovered by the N2K program that worked out of the Magellan telescopes. HD 154672 b was later observed by a different team of astronomers investigating the role of metallicity, or the amount of metal present in a star, in the formation of planets. Six radial velocity measurements of the host star, collected using the HARPS instrument at Chile's La Silla Observatory. The team used the radial velocity data to refine the parameters of HD 154672 b from what was published in its
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HD 175541 b


HD 175541 b is a jovian planet located approximately 410 light-years away in the constellation of Serpens, orbiting the star HD 175541. This planet was discovered in April 2007. Despite the distance of planet to star slightly more than Earth to the Sun, the period is less than 300 days that orbits in an eccentric orbit, because the parent star is 65% more massive than our Sun. The discovery of this planet and two others: HD 192699 b and HD 210702 b around intermediate-mass stars provide clues about
17565009
HD 106906 b


this process; binary stars typically do not exceed a ratio of 10:1. This is still considered preferable, however, to the alternate theory that the companion formed closer to its primary and then was scattered to its present distance by gravitational interaction with another orbital object. This second companion would need to have a mass greater than that of , and the discovery team found no such object beyond 35 AU from the primary. Additionally, the scattering process would have likely disrupted the protoplanetary disk. Subsequently, astronomer Paul Kalas and colleagues discovered
15791558
Super-Earth


water. By November 2009, a total of 30 super-Earths had been discovered, 24 of which were first observed by HARPS. Discovered on 5 January 2010, a planet HD 156668 b with a minimum mass of 4.15 Earth masses, is the least massive planet detected by the radial velocity method. The only confirmed radial velocity planet smaller than this planet is Gliese 581e at 1.9 Earth masses (see above). On 24 August, astronomers using ESO's HARPS instrument announced the discovery of a planetary system with up to
9653268
HD 89345 b


The parent planet star of about 5.3 billion years old belongs to the spectral class G5V-G6V; it is 66 percent larger and 22 percent more massive than the Sun, and is 413 light-years away. The effective temperature of the star is 5609 Kelvin, and considering that HD 89345 b makes one revolution around the star in 11.8 days, being from it at a distance of 0.11 astronomical unit, This planet was described by researchers as a warm subterranean with an equilibrium temperature of 1059 Kelvin. HD 89345 b,
20305439
HD 40307 b


determine whether a protostar's accretion disk forms gas giants or terrestrial planets. The Arizonan astronomer Rory Barnes's mathematical model, in 2009, found that "Planet b’s orbit must be more than 15◦ from face-on"; however it cannot be much more. HD 40307 b does not transit and has not been imaged. More specific characteristics, such as its radius, composition, and possible surface temperature cannot be determined. With a lower mass bound of 4.2 times the mass of the Earth, HD
21995404
HD 164922


Way. The designation "b" derive from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of HD 164922, only one was discovered, which was designated "b", then a more inner planet, which was designated "c". The name HD 164922 derives directly from the fact that the star is the 164,922nd star discovered in the Henry Draper catalog. HD 164922 is a
17426665
HD 61005


matter, forming a planetary system. HD 61005 is located in the Local Bubble - a region with a low concentration of dust clouds. HD 61005 is 115 light years from earth, has an apparent magnitude of 8.23 and a metallicity of 72.4% of the Sun. It is moving through the interstellar medium at a speed of 27.4 km/s relative to the Sun and is found in the night sky at right ascension 113.94248° and declination -32.20°. In 2007, a team of astronomers announced the discovery of a protoplanetary
17953474
HD 80606 b


Geneva Extrasolar Planet Search team using the ELODIE spectrograph mounted on the 1.93-m telescope at the Haute-Provence Observatory. The discovery of HD 80606 b was announced on April 4, 2001. HD 80606 b has the most eccentric orbit of any known planet after HD 20782 b. Its eccentricity is 0.9336, comparable to Halley's Comet. The eccentricity may be a result of the Kozai mechanism, which would occur if the planet's orbit is significantly inclined to that of the binary stars. This interpretation is supported by measurements of the Rossiter
17974682
HD 40307 b


other extrasolar planets, HD 40307 b was discovered by measuring variations in the radial velocity of the star it orbits. These measurements were made by the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph at the Chile-based La Silla Observatory. The discovery was announced at the astrophysics conference that took place in Nantes, France between 16 and 18 June 2008. HD 40307 b was one of three found here at the time. HD 40307 b is the second lightest planet discovered in the system, with at least 4.2 times
21995402
HD 113766


being potentially interesting by Backman et al. using observations made by the Infrared Astronomical Satellite (IRAS) in 1983. Later measurements in 2001 by a team led by Meyer et al. determined that the system was actually a close binary, with the second star in the system, HD 113766 B, a near twin of HD 113766 A orbiting approximately 170 AU from the A star where the terrestrial planet is forming. Located at more than 4 times the distance of Pluto from our own Sun, HD 113766 B has almost no
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HD 8574 b


that had been discovered by ELODIE at the same time). HD 8574 b was announced by the European Southern Observatory on April 4, 2001. The findings addressing HD 8574's discovery were published in 2003. HD 8574 is an F-type dwarf star that lies 45 parsecs (146 light years) away from Earth. HD 8574 has an estimated mass of 1.17 times the mass of the Sun. The star also has a radius that is estimated at 1.37 times that of the Sun's. HD 8574 has an effective
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HD 142527


HD 142527 is a star in the constellation of Lupus. It is notable for its protoplanetary disk and its discovery has helped refine models of planet formation. HD 142527 is an extremely young star, aged about 1 million years old so it retains its protoplanetary disk which has a mass of 15% of the mass of the Sun and a diameter of 980 AU. The studies have shown eddies and vortex structures forming in the nebulae under the influence of two large planets. The star is important as it allows Astronomers to observe the
21084414
HD 102956 b


designated as the planet that will be named by Sweden. The designation b derive from the order of discovery. The designation of b is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of HD 102956, only one was discovered, which was designated b, a 2nd planet would be designated c. The star itself has the designation a, although this is seldom used. The name HD 102956 derives directly from the fact that the star is the 102,956th star
10264503
HD 122430 b


HD 122430 b is a giant planet orbiting around the giant star HD 122430. It has a mass at least 3.71 times that of Jupiter. This planet located at a distance of 1.02 astronomical units away from its star, which is very similar to the Earth's distance from the Sun. Despite of this, the higher luminosity of the star implies it is heated much more strongly than the Earth is. Its orbit is highly eccentric, around 68%. At periastron, the orbital distance from its parent star is 0.33 AU
17565098
HD 209458 b


HD 209458 b, also given the nickname Osiris, is an exoplanet that orbits the solar analog HD 209458 in the constellation Pegasus, some 159 light-years from the Solar System. The radius of the planet's orbit is 7 million kilometres, about 0.047 astronomical units, or one eighth the radius of Mercury's orbit. This small radius results in a year that is 3.5 Earth days long and an estimated surface temperature of about 1,000 °C (about 1,800 °F). Its mass is 220 times that of Earth
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HD 41004


HD 41004 is a star system approximately 139 light years away in the constellation of Pictor. HD 41004 A is a primary orange dwarf star of spectral type K1V and apparent magnitude 8.65. In 2003 a planet HD 41004 Ab was first discovered by Zucker, but not published until 2004. It has a mass 2.56 times that of Jupiter. It orbits at 1.70 astronomical units, taking 963 days, with 74% eccentricity. HD 41004 B is a red dwarf with spectral type M2V and apparent magnitude 12.33. HD 41004 Bb is
11737864
HD 128311


HD 128311 or HN Boötis is an orange main-sequence star located approximately 54 light-years away in the constellation of Boötes. Two extrasolar planet candidates have been detected in orbit around this star. In 2002, the discovery of the planet HD 128311 b was announced by Paul Butler. In 2005, the discovery of a second planet HD 128311 c was announced by Steve Vogt. Most likely, the system has been formed in a very turbulent disc. The authors were able to show with both analytic and numerical models that
9282008
HD 205739 b


the Magellan Inamori Kyocera Echelle spectrograph's (MIKE) ability to use Doppler spectroscopy to measure radial velocity. Twenty-four measurements were recorded for HD 205739. The measurements were analyzed for accuracy. They were then used to derive the planet's characteristics, which led to the planet's confirmation. The team of astronomers, which were from the United States, Chile, and the Vatican City, sent the paper to the "Astronomical Journal" on April 7, 2008. The paper was accepted, and was later published on
16181747
HD 204313 b


HD 204313 b is an extrasolar planet which orbits the G-type main sequence star HD 204313, located approximately 155 light years away in the constellation Capricorn. This planet orbits the star at a distance of 3.082 astronomical units and takes 1931 days or 5.29 years to revolve around the star. It has minimum mass four times that of Jupiter. However the radius and inclination are not known since this planet was not detected by transit method or direct imaging. Instead, this planet was detected by radial velocity method using the CORALIE Echelle
12481117
HD 83443


be slightly larger than Jupiter in radius. In 2000, the same year that planet b was found, another planet around HD 83443 was announced by the Geneva Team. The new planet was designated as "HD 83443 c". It had a mass smaller than planet b and a short, very eccentric orbit. Its orbital period, 28.9 days, was especially interesting, because it indicated a 10:1 orbital resonance between the planets. However, a team led by astronomer Paul Butler did not detect any signal indicating the existence of
17246996
HD 1237


around its axis more quickly than the Sun. The secondary star was discovered in 2006 during a deep imaging survey conducted at the European Southern Observatory using the Very Large Telescope. HD 1237 B is a M4 red dwarf star at a projected separation of 68 AU. Announced in 2000, the Jovian planet GJ 3021 b (GJ 3021 being an alternate less-used designation for this star) orbits about 0.5 astronomical units from HD 1237 A with a minimum mass 3.37 times that of Jupiter, as determined by measuring variations in the
19344707
HD 40307 b


the mass of the Earth. The planet orbits the star HD 40307 every 4.3 Earth days, corresponding of its location at approximately 0.047 astronomical units from the star. The eccentricity of the planet's orbit was found to not differ significantly from zero, meaning that there is insufficient data to distinguish the orbit from an entirely circular one. The star around which HD 40307 b orbits has a low metallicity, compared to other planet-bearing stars. This supports a hypothesis concerning the possibility that the metallicity of stars during their births may
21995403
HD 143361 b


HD 143361 b is an extrasolar planet located approximately 194 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 is not known, the true mass is 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
3338422
HD 240237


HD 240237 is a red giant approximately 4,900 light-years away in the constellation Cassiopeia. The star has an exoplanet orbiting around it every 745 days. The designation "b", derives from the order of discovery. The designation of "b" is given to the first planet orbiting a given star, followed by the other lowercase letters of the alphabet. In the case of HD 240237, there was only one planet, so only the letter "b" is used. The star is known to host one planet
3919896
51 Pegasi b


' have been discovered (see 55 Cancri and τ Boötis, for example), and astronomers are revising their theories of planet formation to account for them by studying orbital migration. Assuming the planet is perfectly grey with no greenhouse or tidal effects, and a Bond albedo of 0.1, the temperature would be 1265 K (approximately 1000 °C / 1800 °F). This is between the predicted temperatures of HD 189733 b and HD 209458 b (1180–1392 K), before they were measured. In the report of the
21487816
Hot Jupiter


or SPIs. The HD 189733 system is the best-studied exoplant system where this effect was thought to occur. In 2008, a team of astronomers first described how as HD 189733 b reaches a certain place in its orbit, it causes increased stellar flaring in its host star. In 2010, a different team found that every time they observe the exoplanet at a certain position in its orbit, they also detected X-ray flares. In 2019, astronomers combined data from Arecibo Observatory, MOST, and the Automated Photoelectric
7439473
HD 217107 b


HD 217107 b is an extrasolar planet approximately 65 light-years away from Earth in the constellation of Pisces (the Fish). The planet was discovered orbiting the star HD 217107 approximately every seven days, classifying the planet as a hot Jupiter. Because of the planet's somewhat eccentric orbit, scientists were able to confirm another planet within the system (HD 217107 c). As with the majority of extrasolar planet discoveries so far, it was found by detecting small variations in the radial velocity of the star it orbits,
11126772
HD 8574 b


factor that could mask or mimic the signal of an orbiting planet. It was found that the star was not significantly active. In the case of HD 8574, ELODIE obtained 41 radial velocity measurements, which had, at the time of the discovery paper, been collected since January 11, 1998. Analysis of the collected data confirmed the existence of a planet orbiting HD 8574. Of the six, the planet HD 8574 b had the shortest orbital period, orbiting its host star under three years (unlike the five other planets
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HD 153950 b


the other hand, this mass can be distributed into many small satellites as well. HD 153950's designation is from the Henry Draper catalogue. The star was also observed by "Hipparcos", which released its catalogue in 1997. The observations that led to the discovery of the planet HD 153950 b started when the N2K Consortium started an extended search for planets around 300 stars not usually targeted by Doppler spectroscopy surveys. In the case of HD 153950, the star was observed using telescopes at the La Silla Observatory in Chile
3338420
HD 209458


HD 209458 is V376 Pegasi. It is the prototype of the variable class "EP" in the General Catalogue of Variable Stars, defined as stars showing eclipses by their planets. HD 209458 b is an extrasolar planet that orbits the Sun-like star HD 209458 in the constellation Pegasus. Spectroscopic studies first revealed the presence of a planet around HD 209458 on November 5, 1999. The planet is now under even more public scrutiny with the announcement that its atmosphere contains water vapor. Astronomers had made careful photometric measurements of several
21261528
HD 7924 b


of . When HD 7924 b was discovered in 2009, it was one of only eight planets known with a minimum mass less than 10 Earths. Also a super-Earth discovery makes 2009 the fifth year in a row since 2005 to have super-Earth planets discovered. While the radius of HD 7924 b is unknown, depending on its composition, it will be between 1.4–6 times the diameter of the Earth. It is unknown whether this planet is rocky or gaseous. Since the true mass of this planet is not known
9039797
Discovery HD


Discovery HD is the international name of the high-definition television channels from Discovery Communications. The international Discovery HD (now Discovery HD World in Asia-Pacific markets) first launched in Korea in February 2005 as a programming block. In December 2005, Discovery HD Japan and Discovery HD Canada (since renamed Discovery World HD) launched as 24-hour channels, becoming the 100th and 101st Discovery networks overall. After this, Discovery HD expanded into other markets as follows: The first American HD Discovery channel has the name Velocity and launched
17971936
HD 82943


HD 82943 (164 G. Hydrae) is a yellow dwarf star approximately 89 light-years away in the constellation of Hydra. Two extrasolar planets have been confirmed to be orbiting it, and it is thought that the system had more giant planets that were "swallowed" by the parent star. HD 82943 is estimated at roughly 1.15 times the mass of the Sun. The first planet discovered (designated HD 82943 b) was announced in 2000 by a team of French astronomers led by Michel Mayor. The planet orbits its parent
21022763
Aquarius (constellation)


, is host to one exoplanet, WASP-6 b. The star is 307 parsecs from Earth and has a mass of 0.888 solar masses and a radius of 0.87 solar radii. WASP-6 b was discovered in 2008 by the transit method. It orbits its parent star every 3.36 days at a distance of 0.042 astronomical units (AU). It is 0.503 Jupiter masses but has a proportionally larger radius of 1.224 Jupiter radii. HD 206610, a K0 star located 194 parsecs from Earth, is host to one planet, HD 206610 b. The
218195
HD 2638


HD 2638 is a dim 10th magnitude star in the constellation of Cetus. It is a yellow dwarf and similar to our Sun. A small telescope is required to view the star. HD 2638 is in a system with multiple stars, including at least HD 2567 and HD 2638 C. HD 2638 is 180 light-years (55 parsecs) from the Sun. In 2005 the discovery of an extrasolar planet HD 2638 b orbiting the star was announced by the Geneva Extrasolar Planet Search Team. The planet has a mass 0.48 of
17464411
HD 40307 c


kind of planets they will form. Like the other two exoplanets, HD 40307 b and HD 40307 d, orbiting the star HD 40307, HD 40307 c was discovered by measuring variations in the radial velocity of HD 40307 caused by the star's orbit around the center of mass of the planetary system. These measurements were made by the High Accuracy Radial Velocity Planet Searcher spectrograph apparatus (HARPS) at the La Silla Observatory in Chile's Atacama Desert. The discovery of planets in the HD 40307 system was announced in an astrophysics
21995407
Gliese 3634 b


targeted by astronomers in search of planets that may orbit such stars. Using the High Accuracy Radial Velocity Planet Searcher (HARPS) at La Silla Observatory in Chile, six years of radial velocity data led the astronomers in the discovery of eleven other planets. After these discoveries, the astronomers chose to refocus their search on short-period planets, hoping to follow up after discoveries using the radial velocity method with a search for planets that also transited, or crossed in front of, their host stars as seen from Earth. The
7334393
HD 154672 b


gaseous and liquid phases as the planet moves along its orbit. The high eccentricity of the planet's orbit suggests that either the Kozai mechanism (there is an exchange between the inclination of a planet and its eccentricity) is at work, or that the planet's orbit was distorted by the unstable orbit of other planets that used to be part of the HD 154672 system. HD 154672 b had, at the time of its 2008 discovery, an orbital period larger than 90% of all discovered planets. It was the seventh
16181726
55th Air Defense Artillery Regiment


Bn HHBs were activated at Ft. Ruger 5-22-43. Btry G (SL) was activated at Ft. Kamehameha. The 1st Bn HHB and Btrys A, B, & C, and 2nd Bn HHB were stationed at Ft. Kamehameha, Btry D on Kauai, Btry E at Wilridge. A detachment from Btry F was at Sand Is. The 811th CA (HD) Btry (Sep) was activated 8-1-42, at Hilo, HI, with personnel from Btry B. In September
11111740
HD 40307 d


method, which functions by measuring the variations in radial velocity in a star produced by the gravitational effect of orbiting exoplanets. The radial velocities were measured by the High Accuracy Radial Velocity Planet Searcher spectrography system (HARPS) at the La Silla Observatory in Chile's Atacama Desert. The other less massive planets orbiting HD 40307 were discovered in the same way: HD 40307 b and HD 40307 c first, and then HD 40307 e, HD 40307 f, and HD 40307 g. The discovery of HD 40307 d and the former two
21995412
HD 38529


least 86 astronomical units from the star. In 2002, the planet HD 38529 b was discovered orbiting the star HD 38529 A by Debra Fischer who used Doppler spectroscopy. It has mass 78% that of Jupiter and orbits very close to the star, just beyond the distance limit for hot Jupiters. One year later, a massive superjovian HD 38529 c was found orbiting at 3.68 AU with a minimum mass of 12.7 Jupiter masses. Astrometric measurements from the Hipparcos satellite gave a best fit inclination of 160° and a true mass
4194576
HD 196050 b


HD 196050 b is a 1378-day extrasolar planet with a minimum mass of 2.90 Jupiter mass. The average orbital distance is 2.54 astronomical units or 380 gigameters or 12.3 microparsecs. The orbital eccentricity is 22.8%. The periastron (closest) distance is 1.96 AU and the apastron (farthest) distance is 3.12 AU. The average orbital velocity is 20.1 km/s and the semi-amplitude is 49.7 m/s. The longitude of periastron is 187° and the time of periastron is 2,450,843 JD. The planet is typically discovered
17565063
Maciej Konacki


Dr. Maciej Konacki (MATCH-ee Konn-ATZ-kee) (born 1972 in Toruń, Poland) is a Polish astronomer, notable for his tentative discovery of HD 188753 Ab, a possible planet discovered in a three star system. The planet would be similar to Jupiter. Konacki received a Master of Science degree in astronomy in 1996 and a Ph.D. in astronomy in 2000, all at Nicolaus Copernicus University Dr. Konacki tentatively discovered HD 188753 Ab with the Keck I telescope on top of Mauna Kea mountain in Hawaii. The
20885358
HD 134606


, having a chromospheric activity index of −5.04. It has about the same mass as the Sun but is 25% more luminous. The photosphere is radiating energy at an effective temperature of 5,614 K. It has a higher than solar metallicity rating – a term astronomers use to describe the abundance of elements other than hydrogen and helium. The discovery of a planetary system orbiting HD 134606 was announced in 2011 following an eight-year survey carried out at the La Silla Observatory in Chile. The detection was made via the radial velocity method
21323269
HD 164427


the 3.92m Anglo-Australian Telescope. A magnitude 12.60 companion star designated lies at an angular separation of along a position angle of 336°, as of 2010. This is a suspected common proper motion companion with 52% of the Sun's mass and a physical separation of as much as . HD 164427 b is a brown dwarf with a minimum mass of 46 times that of Jupiter. It orbits at nearly half an astronomical unit or Earth-to-Sun distance away from its star (HD 164427). The
619568
HD 154345 b


HD 154345 b, is a Jupiter-sized extrasolar planet orbiting the star HD 154345. Wright et al. discovered the planet in March 2006 using the radial velocity method to detect the small wobbling movement of the star caused by the gravity of the planet. The discovery was confirmed in May 2007. The planet has a mass at least slightly less than that of Jupiter. It orbits its parent star at the distance of 4.18 AU. Its orbital period is about 9.095 Earth years and its orbit is circular. There are no
4116243
HD 154672


HD 154672 is a yellow subgiant (spectral type G3 IV). It is about 65 parsecs away from the Sun that is larger than, but of a similar mass to, the Sun. However, HD 154672 is much older. The star is very metal-rich, which is one of the reasons why it was targeted for a planet search by the N2K Consortium, which discovered the gas giant planet HD 154672 b using Doppler Spectroscopy; the discovery was reported in October 2008. The N2K collaboration chose HD
7560063
HD 96700


from orbiting objects. The innermost planet, HD 96700 b, is orbiting close to the star at a distance of roughly 0.08 AU with a brief orbital period of 8.13 days. It has at least nine times the mass of the Earth, and so may be a Neptune-like planet. But until astronomers can determine the orbital inclination or directly image the planet, there is no way to know for certain its actual mass. The second companion, HD 96700 c, is orbiting at roughly the same distance as Mercury from
10719707
HD 149026 b


of 0.3 had come from averaging Sudarsky's theoretical classes IV and V. The planet's extremely high temperature has forced astronomers to abandon that estimate; now, they predict that the planet must absorb essentially all of the starlight that falls on it — that is, effectively zero albedo like HD 209458 b. Much of the absorption takes place at the top of its atmosphere. Between that and the hot, high-pressure gas surrounding the core, a stratosphere of cooler gas was once predicted but has not been observed. The atmosphere is
12289330
HD 189733 b


observed, approximately 3%. The apparent longitude of ascending node of its orbit is 16 degrees +/- 8 away from north-south in our sky. It and HD 209458 b were the first two planets to be directly spectroscopically observed. The parent stars of these two planets are the brightest transiting-planet host stars, so these planets will continue to receive the most attention by astronomers. Like most hot Jupiters, this planet is thought to be tidally locked to its parent star, meaning it has a permanent day and
14602778
HD 142415 b


HD 142415 b is an exoplanet with the semi-amplitude of 51.3 ± 2.3 m/s. This indicates the minimum mass of 1.69 Jupiter mass, an orbital period of 386.3 days, and the semi-major axis of 1.07 astronomical units based from its stellar mass. The wild, oval pathed wobble of the star used by Doppler spectrometer indicates that the orbit of the planet is highly eccentric at around 50%. The planet was discovered in La Silla Observatory on 30 June 2003 by Mayor, who used the CORALIE spectrograph
17974727
HD 209458 b


one part of the infrared spectrum, compared to wavelengths in the visible spectrum. Barman took Knutson's Hubble data on HD 209458 b, applied to his theoretical model, and allegedly identified water absorption in the planet's atmosphere. On April 24, the astronomer David Charbonneau, who led the team that made the Hubble observations, cautioned that the telescope itself may have introduced variations that caused the theoretical model to suggest the presence of water. He hoped that further observations would clear the matter up in the following months. As of
7889755
Discovery Asia


Discovery Asia (formerly as Discovery HD and Discovery HD World) is a Southeast Asian pay television channel that features Asia-related documentaries and original Asian programming. It is operated by Discovery Asia-Pacific, a division of Discovery, Inc. The channel was launched in 2005 as Discovery HD, the first high-definition channel in Asia. It was first available in South Korea in February, and in Japan in December. On April 1, 2010, Discovery HD was rebranded to Discovery HD World. In 2008, Discovery Channel
18566103
HD 65216 b


HD 65216 b is an extrasolar planet located approximately 116 light-years away in the constellation of Carina, orbiting the star HD 65216. This planet was discovered by the Geneva Extrasolar Planet Search Team in 2003. Like most planet candidates so far, it was detected with the radial velocity method. The planet has a minimum mass about 20% more than Jupiter. Since the discovery method gives only the minimum mass, its true mass is probably slightly greater. The planet orbits the star in a very eccentric orbit. The mean
17974666
HD 156668 b


HD 156668 b is an extrasolar planet orbiting the star HD 156668 78.5 light-years away in the constellation Hercules. It has a minimum mass of 3.1 Earth masses. At the time of discovery it was the second least massive planet discovered by the radial velocity method, subject to the mass/inclination degeneracy that affects radial velocity measurements. The only radial velocity planet less massive than this planet is Gliese 581 e, which was discovered on April 21, 2009, and has a minimum mass of 1.94 Earth masses. In addition
21464612
HD 221287


HD 221287 is a yellow-white main-sequence star approximately 173 light years away in the constellation of Tucana. It has an apparent magnitude of 7.82 and absolute magnitude of 4.20. This star is also named HIP 116084. On March 5, 2007, the astronomer Dominique Naef used the HARPS spectrograph to uncover HD 221287 b (among others). Using the amplitude from observations with HARPS, he calculated a minimum mass of 3.12 times that of Jupiter, making this a superjovian. This planet orbits 25% further from the
10788360
HD 98800


2007, a debris disk was discovered orbiting HD 98800 B consisting of two rings which indicates there may be an extrasolar planet orbiting within a distance of 1.5 to 2 astronomical units. The system is a member of the TW Hydrae association, a group of young stars. Its membership was derived from the fact that its proper motion is similar to other stars in the group.The system itself is estimated to be around 7-10 million years old. HD 98800 is a quadruple system, with two pairs of stars orbiting each
11562785
HD 74156


giant planets were announced orbiting the star. The first planet HD 74156 b orbits the star at a distance closer than Mercury is to our Sun, in an extremely eccentric orbit. The second planet HD 74156 c is a long-period, massive planet (at least 8 times the mass of Jupiter), which orbits the star in an elliptical orbit with a semimajor axis of 3.90 astronomical units. Given the two-planet configuration of the system under the assumption that the orbits are coplanar and have masses equal to their minimum
21022756
HD 136118 b


HD 136118 b is a brown dwarf located approximately 171 light-years away in the constellation of Serpens Cauda. This object had a minimum mass of 11.9 times that of Jupiter. Due to its high mass the planet is likely to be very hot and possibly glowing faintly. The lower limit on its mass is only slightly less than the deuterium burning threshold that some astronomers use to distinguish between planets and brown dwarfs. Depending on the inclination of its orbit, the true mass could be above this limit. The orbit of the
10482044
Travis Barman


Travis Barman is an astronomer at the Lowell Observatory in Arizona, in the United States. While studying a combination of the previously published Hubble Space Telescope measurements and new theoretical models, Barman found strong evidence for water absorption in the atmosphere of HD 209458 b. A planet about 150 light years away from earth, HD 209458 b was known previously to contain an evaporating hydrogen atmosphere, along with oxygen and carbon. Though the planet is only 7 million kilometers away from its star, the planet is not hot enough to break the water
2594143
HD 209458 b


" article came out, but made similar findings. On 23 June 2010, astronomers announced they have measured a superstorm (with windspeeds of up to 7000 km/h) for the first time in the atmosphere of HD 209458 b. The very high-precision observations done by ESO’s Very Large Telescope and its powerful CRIRES spectrograph of carbon monoxide gas show that it is streaming at enormous speed from the extremely hot day side to the cooler night side of the planet. The observations also allow another exciting "first"—measuring the orbital speed
7889745
HD 209458 b


measured. This detection was predicted by Sara Seager in late 2001. The core of the sodium line runs from pressures of 50 millibar to a microbar. This turns out to be about a third the amount of sodium at HD 189733 b. In 2003–4, astronomers used the Hubble Space Telescope Imaging Spectrograph to discover an enormous ellipsoidal envelope of hydrogen, carbon and oxygen around the planet that reaches 10,000 K. The hydrogen exosphere extends to a distance "R"=3.1 "R", much larger than the planetary radius of 1.32 R. At this temperature
7889750
HD 149026 b


the Keck and Subaru Telescopes. After the planet was first detected from the Doppler effect it caused in the light of the host star, it was studied for transits at the Fairborn Observatory. A tiny decrease of light (0.003 magnitudes) was detected every time the planet was transiting the star, thus confirming its existence. Although the change of brightness caused by the transiting planet is tiny, it is detectable by amateur astronomers, providing an opportunity for amateurs to make important astronomical contributions. Indeed, one amateur astronomer, Ron Bissinger
12289327
1661 Granule


days). Its orbit has an eccentricity of 0.09 and an inclination of 3° with respect to the ecliptic. "Granule"s observation arc begins with its observation at Bergedorf Observatory, one month after its official discovery observation. (It is unclear whether "HD 17", "Message from Heidelberg Observatory #17", is the official discovery observation due to a different time stamp). In January 2006, the first rotational light-curve of "Granule" was obtained from photometric observations by French amateur astronomer René Roy.
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