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Eos Family
The Eos family (''adj. Eoan'' ; ) is a very large asteroid family located in the outer region of the asteroid belt. The family of K-type asteroids is believed to have formed as a result of an ancient catastrophic collision. The family's parent body is the asteroid 221 Eos. Description In 1918, while the Japanese astronomer Kiyotsugu Hirayama was studying at Yale University, he began to examine asteroid motions. By plotting the mean motion, eccentricity and inclination of the asteroid orbits, he discovered that some of the objects formed groupings. In a 1918 paper, he described three such groups, including the Eos family with 19 members. Since that time, the number of members in the Eos family grouping has continued to grow, reaching 289 by 1993. Currently there are about 4,400 known members of the Eos family. The inner orbit of the family is bracketed by the 7/3 mean-motion resonance with Jupiter at 2.96 AU. The orbital range also includes the 9/4 mean-motion resonance with ... [...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] |
221 Eos
Eos ( minor planet designation: 221 Eos) is a large main-belt asteroid that was discovered by Austrian astronomer Johann Palisa on January 18, 1882, in Vienna. In 1884, it was named after Eos, the Greek goddess of the dawn, to honour the opening of a new observatory that was hoped to bring about a new dawn for Viennese astronomy. The asteroid is orbiting the Sun with a semimajor axis of , a period of 5.22 years, and an eccentricity of 0.1. The orbital plane is inclined by 10.9° to the plane of the ecliptic. It has a mean cross-section of 104 km, and is spinning with a rotation period of 10.4 hours. Based upon its spectral characteristics, this object is classified as a K-type asteroid. The orbital properties show it to be a member of the extensive Eos asteroid family, which is named after it. The spectral properties of the asteroid suggest it may have come from a partially differentiated parent body. References External linksThe Asteroid Orbital Elements D ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
807 Ceraskia
807 Ceraskia ( ''prov. designation'': ''or'' ) is an elongated Eos asteroid from the outer regions of the asteroid belt. It was discovered on 18 April 1915, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany. The S-type asteroid has a rotation period of 7.4 hours and measures approximately in diameter. It was named after Belarusian–Soviet astronomer Vitold Cerasky (1849–1925). Orbit and classification ''Ceraskia'' is a core member the Eos family (), the largest asteroid family of the outer main belt consisting of nearly 10,000 known asteroids. It orbits the Sun in the outer asteroid belt at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,913 days; semi-major axis of 3.02 AU). Its orbit has an eccentricity of 0.07 and an inclination of 11 ° with respect to the ecliptic. The asteroid was first observed as at Heidelberg Observatory on 18 January 1909. The body's observation arc begins at Vienna Obse ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
798 Ruth
798 Ruth is a minor planet orbiting the Sun that was discovered by the German astronomer Max Wolf on 21 November 1914. It may have been named after the biblical character Ruth. This main belt asteroid has an orbital period of and is orbiting at a distance of from the Sun with an eccentricity (ovalness) of 0.036. The orbital plane is tilted by 9.2° from the plane of the ecliptic. This is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. It is an M-type (metallic) asteroid that displays a significant component of the mineral olivine in its spectrum A spectrum (plural ''spectra'' or ''spectrums'') is a condition that is not limited to a specific set of values but can vary, without gaps, across a continuum. The word was first used scientifically in optics to describe the rainbow of colors i .... 798 Ruth spans and rotates on its axis once every . References External links * * 000798 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
742 Edisona
742 Edisona is a minor planet orbiting the Sun that was discovered by German astronomer Franz Kaiser on February 23, 1913. It was named for inventor Thomas Edison. This asteroid is orbiting with a period of and an eccentricity of 0.119. The orbital plane is inclined at an angle of 11.2° to the plane of the ecliptic. This is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. Photometric observations made during 2008 were used to produce a light curve of 742 Edisona showing a rotation period of with a brightness variation of in magnitude Magnitude may refer to: Mathematics *Euclidean vector, a quantity defined by both its magnitude and its direction *Magnitude (mathematics), the relative size of an object *Norm (mathematics), a term for the size or length of a vector *Order of .... It spans a girth of approximately 45.6 km. References External links * * Eos asteroids Edisona ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
669 Kypria
669 Kypria is a minor planet orbiting the Sun that was discovered by German astronomer August Kopff on August 20, 1908. This is a member of the dynamic Eos family The Eos family (''adj. Eoan'' ; ) is a very large asteroid family located in the outer region of the asteroid belt. The family of K-type asteroids is believed to have formed as a result of an ancient catastrophic collision. The family's parent body ... of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links * * Eos asteroids Kypria Kypria S-type asteroids (Tholen) 19080820 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
661 Cloelia
661 Cloelia is a minor planet orbiting the Sun that was discovered by American astronomer Joel Hastings Metcalf on February 22, 1908. Cloelia is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. The planet is named after the Ancient Roman woman Cloelia. The name may have been inspired by the asteroid's provisional designation ''1908 CL''. References External links * * Eos asteroids Cloelia Cloelia Cloelia ( grc, Κλοιλία) was a legendary woman from the early history of ancient Rome. Biography She was one of the women taken hostage by Lars Porsena, as a part of the peace treaty which ended the war between Rome and Clusium in 508 BC. ... S-type asteroids (Tholen) K-type asteroids (SMASS) 19080222 Cultural depictions of Cloelia {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
653 Berenike
653 Berenike is a main-belt asteroid discovered on 27 November 1907 by Joel Hastings Metcalf at Taunton, Massachusetts. It is named after Berenice II of Egypt, after whom the constellation Coma Berenices is also named. The name may have been inspired by the asteroid's provisional designation ''1907 BK''. Berenike is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links * * Eos asteroids Berenike Berenike Berenice ( grc, Βερενίκη, ''Bereníkē'') is the ancient Macedonian language, Ancient Macedonian form of the Attic Greek name ''Pherenikē'', which means "bearer of victory" . Berenika, priestess of Demeter in Lete (Mygdonia), Lete ca. 350 ... S-type asteroids (Tholen) K-type asteroids (SMASS) 19071127 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
651 Antikleia
651 Antikleia is a main-belt asteroid discovered on 4 October 1907 by August Kopff at the Heidelberg-Königstuhl State Observatory. It is named for Anticlea the mother of Odysseus. The name may have been inspired by the asteroid's provisional designation ''1907 AN''. Antikleia is a member of the dynamic Eos family The Eos family (''adj. Eoan'' ; ) is a very large asteroid family located in the outer region of the asteroid belt. The family of K-type asteroids is believed to have formed as a result of an ancient catastrophic collision. The family's parent body ... of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links * * Eos asteroids Antikleia Antikleia S-type asteroids (Tholen) 19071004 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
639 Latona
639 Latona is a minor planet, specifically an asteroid orbiting in the asteroid belt. It was discovered by German astronomer Karl Lohnert on July 19, 1907, at Heidelberg. Photometric observations of this asteroid at Palmer Divide Observatory in Colorado Springs, Colorado, during 2007 gave a light curve with a period of 6.139 ± 0.002 hours and a brightness variation of 0.08 ± 0.01 in magnitude. This confirms period measurements of about 6.2 hours reported in 1987 and 2001. This is a member of the dynamic Eos family of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links Lightcurve plot of 639 Latona Palmer Divide Observatory, '' B. D. Warner'' (2007) Asteroid Lightcurve Database (LCDB) query form) Dictionary of Minor Planet Names Google books – Observatoire de Genève, Raoul Behrend – Minor Planet Center * * Eos asteroids Latona Leto Latona In ancient Greek mythology and religion, Leto (; ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
633 Zelima
633 Zelima 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 ... in the asteroid belt with a magnitude of 10.7. The name may have been inspired by the asteroid's provisional designation ''1907 ZM''. References External links Lightcurve plot of 633 Zelima Palmer Divide Observatory, '' B. D. Warner'' (2006) Asteroid Lightcurve Database (LCDB) query form) Dictionary of Minor Planet Names Google books – Observatoire de Genève, Raoul Behrend – Minor Planet Center * * Eos asteroids Zelima Zelima S-type asteroids (Tholen) S-type asteroids (SMASS) 19070512 {{beltasteroid-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
562 Salome
Salome (minor planet designation: 562 Salome) is a minor planet orbiting the Sun that was discovered by German astronomer Max Wolf on 3 April 1905 from Heidelberg. It is named after Salome, the daughter of Herodias who is referenced in the New Testament.In light of Wolf's propensity at the time to name asteroids after female characters in opera, it is possible that he may have had in mind the rendition of Salome in Richard Strauss's eponymous opera, which premiered in Dresden the year of discovery. This is a member of the dynamic Eos family The Eos family (''adj. Eoan'' ; ) is a very large asteroid family located in the outer region of the asteroid belt. The family of K-type asteroids is believed to have formed as a result of an ancient catastrophic collision. The family's parent body ... of asteroids that most likely formed as the result of a collisional breakup of a parent body. References External links * * 000562 Discoveries by Max Wolf Named minor planets ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
