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Innes' Star
Innes' star (Gliese 422) is an M-type dwarf, M3.5-type red dwarf, located in constellation Carina (constellation), Carina. It has around 35% of the mass of the Sun, yet only 1.1% of its luminosity, and an estimated surface temperature of 3,323 Kelvin, K. Discovery Innes' star was discovered in 1920 by Robert T. A. Innes in Union Observatory, Union of South Africa, who had discerned its large proper motion and a parallax of 0.337 arcsec. The discovery was published in ''Circular of the Union Observatory'' No. 49, hence its discovery name is ''UO 49'', or ''In UOC 49''. However, ''UO'' designations should be used with caution since they are often not unique for each star: the number in the name is the number of ''Circular'', so all stars published in one ''Circular'' have identical names. So, all other newfound stars, published in the 49th ''Circular'', may be named ''UO 49'' too. Erroneous parallax It is known for the fact that it had once been considered one of the neare ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Carina (constellation)
Carina ( ) is a constellation in the southern sky. Its name is Latin for the keel of a ship, and it was the southern foundation of the larger constellation of Argo Navis (the ship ''Argo'') until it was divided into three pieces, the other two being Puppis (the poop deck), and Vela (the sails of the ship). History and mythology Carina was once a part of Argo Navis, the great ship of Jason and the Argonauts who searched for the Golden Fleece. The constellation of Argo was introduced in ancient Greece. However, due to the massive size of Argo Navis and the sheer number of stars that required separate designation, Nicolas-Louis de Lacaille divided Argo into three sections in 1763, including Carina (the hull or keel). In the 19th century, these three became established as separate constellations, and were formally included in the list of 88 modern IAU constellations in 1930. Lacaille kept a single set of Greek letters for the whole of Argo, and separate sets of Latin letter designa ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ejnar Hertzsprung
Ejnar Hertzsprung (; Copenhagen, 8 October 1873 – 21 October 1967, Roskilde) was a Danish chemist and astronomer. Career Hertzsprung was born in Frederiksberg, Denmark, the son of Severin and Henriette. He studied chemical engineering at Copenhagen Polytechnic Institute, graduating in 1898. After spending two years working as a chemist in St. Petersburg, in 1901 he studied photochemistry at Leipzig University for a year. His father was an amateur astronomy, which led to Ejnar's interest in the subject. He began making astronomical observations in Fredericksberg in 1902, and within a few years had noticed that stars with similar spectral type could have widely different absolute magnitudes. In 1909, he took a position at the Göttingen Observatory under director Karl Schwarzschild. In 1911 Hertzsprung developed the Hertzsprung–Russell diagram, independently developed in 1913 by Henry Norris Russell. In 1913 Hertzsprung determined the distances to several Cepheid variable st ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astronomical Unit
The astronomical unit (symbol: au, or or AU) is a unit of length, roughly the distance from Earth to the Sun and approximately equal to or 8.3 light-minutes. The actual distance from Earth to the Sun varies by about 3% as Earth orbits the Sun, from a maximum (aphelion) to a minimum (perihelion) and back again once each year. The astronomical unit was originally conceived as the average of Earth's aphelion and perihelion; however, since 2012 it has been defined as exactly (see below for several conversions). 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. 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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
GJ 422 B
Gliese 422 b is an exoplanet orbiting the red dwarf Gliese 422 (Innes' star). Gliese 422 b was discovered in 2014, and the discovery was confirmed in 2020. It has a minimum mass of about ten times that of Earth. It is located on the inner edge of circumstellar habitable zone (HZ) of Gliese 422, which extends from 0.11 to 0.21 AU. Gliese 422 b's semi-major axis In geometry, the major axis of an ellipse is its longest diameter: a line segment that runs through the center and both foci, with ends at the two most widely separated points of the perimeter. The semi-major axis (major semiaxis) is the long ... is 0.119 AU and its orbital period is 26.161 Earth days. References External links * Giant planets in the habitable zone Exoplanets discovered in 2014 4 Exoplanets detected by radial velocity {{extrasolar-planet-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mega-Earth
A mega-Earth is a proposed neologism for a massive terrestrial exoplanet that is at least ten times the mass of Earth. Mega-Earths would be substantially more massive than super-Earths (terrestrial and ocean planets with masses around 5–10 Earths). The term "mega-Earth" was coined in 2014, when Kepler-10c was revealed to be a Neptune-mass planet with a density considerably greater than that of Earth, though it has since been determined to be a typical volatile-rich planet weighing just under half that mass. Examples Kepler-10c was the first exoplanet to be classified as a mega-Earth. At the time of its discovery, it was believed to have a mass around 17 times that of Earth () and a radius around 2.3 times Earth's (), giving it a high density that implied a mainly rocky composition. However, several follow-up radial velocity studies produced different results for Kepler-10c's mass, all much below the original estimate. In 2017, a more careful analysis using data from multiple di ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Louise Freeland Jenkins
Louise Freeland Jenkins (July 5, 1888 – May 9, 1970) was an American astronomer who compiled a valuable catalogue of stars within 10 parsecs of the sun, as well as editing the 3rd edition of the Yale Bright Star Catalogue. She was born in Fitchburg, Massachusetts. In 1911 she graduated from Mount Holyoke College, then she received a Master's degree in astronomy in 1917 from the same institution. From 1913 to 1915 she worked at the Allegheny Observatory in Pittsburgh, Pennsylvania, Pittsburgh. Afterwards, she was an instructor at Mount Holyoke from 1915 to 1920. About 1921 she moved to Japan, becoming a teacher at the Women's Christian College, a missionary school. She returned to the United States in 1925 after her father died. A year later she returned to teach at a school in Himeji. (Hinomoto Gakuen girl's high school.) In 1932 she returned to the US and became a staff member at Yale University, Yale University Observatory. She was co-editor of the ''Astronomical Journal'' ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Wolf 1061
__NOTOC__ Wolf 1061 (also known as HIP 80824 and V2306 Ophiuchi) is an M-class red dwarf star located about 14.1 light-years away in the constellation Ophiuchus. It is the 36th-closest-known star system to the Sun and has a relatively high proper motion of 1.2 seconds of arc per year. Wolf 1061 does not have any unusual spectroscopic features. The star Wolf 1061 was first cataloged in 1919 by German astronomer Max Wolf when he published a list of dim stars that had high proper motions. Wolf 1061's name originates from this list. A seven years study found no evidence of photometric transits and confirms the radial velocity signals are not due to stellar activity. The habitable zone estimate for the system lies between approximately 0.1 and 0.2 AU from the star. Planetary system In December 2015, a team of astronomers from the University of New South Wales announced the discovery of three planets orbiting Wolf 1061. The planets were detected by analyzing 10 years of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Wolf 359
Wolf 359 is a red dwarf star located in the constellation Leo, near the ecliptic. At a distance of approximately 7.9 light years from Earth, it has an apparent magnitude of 13.54 and can only be seen with a large telescope. Wolf 359 is one of the nearest stars to the Sun; only the Alpha Centauri system (including Proxima Centauri), Barnard's Star, and the brown dwarfs Luhman 16 (WISE 1049-5319) and WISE 0855−0714 are known to be closer. Its proximity to Earth has led to its mention in several works of fiction. Wolf 359 is one of the faintest and lowest-mass stars known. At the light-emitting layer called the photosphere, it has a temperature of about 2,800 K, which is low enough for chemical compounds to form and survive. The absorption lines of compounds such as water and titanium(II) oxide have been observed in the spectrum. The surface has a magnetic field that is stronger than the average magnetic field on the Sun. As a result of magnetic activity caused ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Peter Van De Kamp
Piet van de Kamp (December 26, 1901 in Kampen (Overijssel), KampenLaurence W. Fredrick, Peter van de Kamp (1901–1995)', Publications of the Astronomical Socitiey of the Pacific 108:556–559, July 1996 – May 18, 1995 in Amsterdam), known as Peter van de Kamp in the United States, was a Dutch astronomer who lived in the United States most of his life. He was professor of astronomy at Swarthmore College and director of the college's Sproul Observatory from 1937 until 1972. He specialized in astrometry, studying parallax and proper motions of stars. He came to public attention in the 1960s when he announced that Barnard's star had a planetary system based on observed "wobbles" in its motion, but this is now known to be false. On November 14, 2018, the Red Dots project announced that Barnard's star hosts an exoplanet at least 3.2 times as massive as Earth, though this does not match either of the planets he had claimed. In 2021, even this planet's existence was questioned. Lif ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lalande 21185
Lalande 21185 (also known as BD+36 2147, Gliese 411, and HD 95735) is a star in the south of Ursa Major. It is the apparent brightest red dwarf in the northern hemisphere.Only AX Microscopii and Lacaille 9352, in the southern hemisphere, are brighter Despite this, and being relatively close by, it is (as are all red dwarfs) very dim, being only magnitude 7.5 in visible light and thus too faint to be seen with the unaided eye. The star is visible through a small telescope or binoculars. At approximately away it is one of the stars nearest to the Solar System; only the Alpha Centauri system, Barnard's Star, and Wolf 359 and the brown dwarfs Luhman 16 and WISE 0855−0714 are known to be closer. Because of its proximity it is a frequent subject for astronomical surveys and other research and thus is known by numerous other designations, most commonly Gliese 411 and HD 95735. In approximately 19,900 years it will be at its closest, about 4.65 ly (1.43 pc) from the Su ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Harlow Shapley
Harlow Shapley (November 2, 1885 – October 20, 1972) was an American scientist, head of the Harvard College Observatory (1921–1952), and political activist during the latter New Deal and Fair Deal. Shapley used Cepheid variable stars to estimate the size of the Milky Way Galaxy and the Sun's position within it by using parallax.Bart J. Bok. Harlow Shapely 1885–1972 A Biographical Memoir. National Academy of Sciences In 1953 he proposed his "liquid water belt" theory, now known as the concept of a habitable zone.Richard J. Hugget, ''uGeoecology: an evolutionary approach''. p. 10 Background Shapley was born on a farm five miles outside Nashville, Missouri, to Willis and Sarah (née Stowell) Shapley. He went to school in Jasper, Missouri, but not beyond elementary school. He worked as a journalist after studying at home and covering crime stories as a newspaper reporter for the ''Daily Sun'' in Chanute, Kansas, and intermittently for the ''Times'' of Joplin, Missouri. In Chanu ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Willem Jacob Luyten
Willem Jacob Luyten (March 7, 1899 – November 21, 1994) was a Dutch-American astronomer. "Willem Jacob Luyten", ''Marquis Who's Who'', 2006. Life Jacob Luyten was born in Semarang, Java, at the time part of the Dutch East Indies. His mother was Cornelia M. Francken and his father Jacob Luyten, a teacher of French. At the age of 11 he observed Halley's Comet, which started his fascination with astronomy. He also had a knack for languages, and eventually could speak nine. In 1912 his family moved back to the Netherlands where he studied astronomy at the University of Amsterdam, receiving his BA in 1918. He was the first student to earn his PhD (at the age of 22) with Ejnar Hertzsprung at Leiden University. In 1921 he left for the United States where he first worked at the Lick Observatory. From 1923 to 1930 Luyten worked at the Harvard College Observatory eventually working at the observatory's Bloemfontein station. He spent the years 1928–1930 in Bloemfontein, South ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
