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Maria Family
The Maria family (adj. ''Marian''; FIN: 506; also known as ''Roma family'') is a collisional asteroid family located in the inner parts of the intermediate asteroid belt, near the 1:3 Kirkwood gap. The family consist of several thousand stony S-type asteroids. It is named after its parent body and lowest numbered member, the asteroid 170 Maria. It is also known as the Roma family, named after its alternative parent body, 472 Roma. The family was initially identified by Japanese astronomer Kiyotsugu Hirayama in 1918. Asteroids in this family typically have a semi-major axis between 2.52−2.62 AU, and an inclination of 12 to 17 °. Members The family consists of 2940 known members based on the HCM method. Its largest members are the asteroids 170 Maria and 472 Roma. A complete synthetic HCM-listing for all members can be obtained by using the ''Ferret Interactive Search''. Interlopers Although asteroid 695 Bella has orbital properties that make it a candid ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Family Identification Number
An asteroid family is a population of asteroids that share similar proper orbital elements, such as semimajor axis, eccentricity (orbit), eccentricity, and orbital inclination. The members of the families are thought to be Collisional family, fragments of past asteroid collisions. An asteroid family is a more specific term than list of minor-planet groups, asteroid group whose members, while sharing some broad orbital characteristics, may be otherwise unrelated to each other. General properties Large prominent families contain several hundred recognized asteroids (and many more smaller objects which may be either not-yet-analyzed, or not-yet-discovered). Small, compact families may have only about ten identified members. About 33% to 35% of asteroids in the main belt are family members. There are about 20 to 30 reliably recognized families, with several tens of less certain groupings. Most asteroid families are found in the main belt, main asteroid belt, although several famil ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Semimajor 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 longest semidiameter or one half of the major axis, and thus runs from the centre, through a focus, and to the perimeter. The semi-minor axis (minor semiaxis) of an ellipse or hyperbola is a line segment that is at right angles with the semi-major axis and has one end at the center of the conic section. For the special case of a circle, the lengths of the semi-axes are both equal to the radius of the circle. The length of the semi-major axis of an ellipse is related to the semi-minor axis's length through the eccentricity and the semi-latus rectum \ell, as follows: The semi-major axis of a hyperbola is, depending on the convention, plus or minus one half of the distance between the two branches. Thus it is the distance from the center t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
695 Bella
695 Bella is a minor planet orbiting the Sun. Although this asteroid has dynamic properties that make it a candidate for the Maria family, the spectral properties of the object indicate it is most likely an interloper. Instead, it may have been spalled off from 6 Hebe or its parent body. 695 Bella and 6 Hebe orbit on opposite sides of the 3:1 Kirkwood gap, and the two have similar orbital elements. References External links * * Maria asteroids Bella Bella Bella is a feminine given name. It is a diminutive form of names ending in -bella. ''Bella'' is related to the Italian, Spanish, Greek, Portuguese and Latin words for beautiful, to the name Belle, meaning ''beautiful'' in French. It increased in ... S-type asteroids (Tholen) 19091107 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
3066 McFadden
3066 McFadden, provisional designation ', is a stony background asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 1 March 1984, by American astronomer Edward Bowell at the Anderson Mesa Station near Tucson, Arizona. It was named for American planetary scientist Lucy-Ann McFadden. The assumed S-type asteroid has a rotation period of 13.8 hours. Orbit and classification ''McFadden'' is a non-Asteroid family, family asteroid from the main belt's Background asteroid, background population. It orbits the Sun in the Kirkwood gap, central asteroid belt at a distance of 2.2–2.9 Astronomical unit, AU once every 4 years (1,466 days; semi-major axis of 2.53 AU). Its orbit has an orbital eccentricity, eccentricity of 0.13 and an orbital inclination, inclination of 16Degree (angle), ° with respect to the ecliptic. The asteroid was first observed as ' at the Simeis Observatory in June 1933. The body's observation arc begins ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
2089 Cetacea
89 may refer to: * 89 (number) 89 (eighty-nine) is the natural number following 88 and preceding 90. In mathematics 89 is: * the 24th prime number, following 83 and preceding 97. * a Chen prime. * a Pythagorean prime. * the smallest Sophie Germain prime to start a Cunnin ... * Atomic number 89: actinium Years * 89 BC * AD 89 * 1989 * 2089 * etc. See also * * List of highways numbered {{Numberdis ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1215 Boyer
1215 Boyer, provisional designation , is a stony Eunomian asteroid from the central region of the asteroid belt, approximately 20 kilometers in diameter. It was discovered by astronomer Alfred Schmitt in 1932, who named it after French astronomer and college Louis Boyer. Discovery ''Boyer'' was discovered on 19 January 1932, by French astronomer Alfred Schmitt at the Algiers Observatory in Algeria, North Africa. Eight days later, it was independently discovered by Karl Reinmuth at Heidelberg Observatory in Germany. The body's observation arc begins at Algiers with its official discovery observation. Classification and orbit ''Boyer'' is a member of the Eunomia family (), the most prominent family in the intermediate main-belt, which mostly consists of stony asteroids. Conversely, ''Boyer'' has also been grouped into the Maria family (). It orbits the Sun at a distance of 2.2–2.9 AU once every 4 years and 2 months (1,512 days). Its orbit has an eccentricity of 0.1 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1158 Luda
1158 Luda, provisional designation , is a stony asteroid from the middle regions of the asteroid belt, approximately 19 kilometers in diameter. It was discovered on 31 August 1929, by Soviet astronomer Grigory Neujmin at Simeiz Observatory on the Crimean peninsula. It was named after Ludmilla Neujmin, the sister of the discoverer. Orbit and classification ''Luda'' orbits the Sun at a distance of 2.3–2.9 AU once every 4 years and 1 month (1,499 days). Its orbit has an eccentricity of 0.11 and an inclination of 15 ° with respect to the ecliptic. The body's observation arc begins with its first used observation at Johannesburg Observatory, one month after its official discovery observation at Simeiz. ''Luda'' is a stony S-type asteroid. Based on its orbital elements, ''Luda'' is a member of the Eunomia family, a large group of stony asteroids and the most prominent family in the intermediate main-belt, while Argentine astronomer Alvarez-Candal from the Universidad Nacio ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
897 Lysistrata
897 Lysistrata is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf Maximilian Franz Joseph Cornelius Wolf (21 June 1863 – 3 October 1932) was a German astronomer and a pioneer in the field of astrophotography. He was the chairman of astronomy at the University of Heidelberg and director of the Heidelberg-Kà ... on August 3, 1918. This is a member of the dynamic Maria family of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links * * 000897 Discoveries by Max Wolf Named minor planets Aristophanes 000897 000897 19180803 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
879 Ricarda
879 Ricarda is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on July 22, 1917. This is a member of the dynamic Maria family of asteroids that most likely formed as the result of a collisional breakup of a parent body. It is named after German intellectual Ricarda Huch Ricarda Huch (; 18 July 1864 – 17 November 1947) was a pioneering German intellectual. Trained as an historian, and the author of many works of European history, she also wrote novels, poems, and a play. Asteroid 879 Ricarda is named in her hono .... Main-belt asteroid 8847 Huch is also named after her. References External links * * 000879 Discoveries by Max Wolf Named minor planets 19170722 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
875 Nymphe
875 Nymphe is a minor planet orbiting the Sun The Sun is the star at the center of the Solar System. It is a nearly perfect ball of hot plasma, heated to incandescence by nuclear fusion reactions in its core. The Sun radiates this energy mainly as light, ultraviolet, and infrared radi .... It is a member of the Maria family of asteroids. References External links Lightcurve plot of 875 Nymphe Palmer Divide Observatory, B. D. Warner (2003) Asteroid Lightcurve Database (LCDB) query form) Dictionary of Minor Planet Names Google books – Observatoire de Genève, Raoul Behrend – Minor Planet Center * * 000875 Discoveries by Max Wolf Named minor planets 19170519 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
787 Moskva
787 Moskva is a minor planet orbiting the Sun. It is a dynamic member of the Maria asteroid family orbiting near the 3:1 Kirkwood gap. This is an S-type (stony) asteroid spanning 27 km. The surface mineralogy is consistent with mesosiderite silicates. Object 1914 UQ, discovered 20 April 1914 by Grigory Neujmin, was named 787 Moskva, after the capital of Russia, Moscow (and retains that name to this day). Object 1934 FD discovered on 19 March 1934 by C. Jackson was given the sequence number 1317. In 1938, G. N. Neujmin found that asteroid 1317 and 787 Moskva were, in fact, the same object. Sequence number 1317 was later reused for the object 1935 RC discovered on 1 September 1935 by Karl Reinmuth; that object is now known as 1317 Silvretta. Photometric observations at the Palmer Divide Observatory in Colorado Springs, Colorado in 1999 were used to build a light curve for this object. The asteroid displayed a rotation period of 6.056 ± 0.001 hours and a brightness variat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
714 Ulula
714 Ulula is a main belt asteroid. It is orbiting the Sun near the 3:1 Kirkwood Gap with a period of 4.04 years and an eccentricity of 0.057. It was discovered by German astronomer J. Helffrich on 18 May 1911 from the Heidelberg Observatory and was named after an order of owls. The asteroid has a mean radius of 20 km and is spinning with a rotation period of seven hours. Its pole of rotation lies just 4–14° away from the plane of the ecliptic. The surface spectrum shows a pyroxene chemistry and is consistent with mesosiderites/HED meteorite HED meteorites are a clan (subgroup) of achondrite meteorites. HED stands for "howardite–eucrite–diogenite". These achondrites came from a differentiated parent body and experienced extensive igneous processing not much different from the magm ...s. References External links * * Maria asteroids Ulula Ulula S-type asteroids (Tholen) 19110518 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
