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1275 Cimbria
1275 Cimbria ( ''prov. designation'': ) is a Eunomia asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 30 November 1932, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southern Germany. The asteroid was named after the Cimbri, an ancient Germanic tribe. Orbit and classification ''Cimbria'' is a member of the Eunomia family (), a prominent family of typically stony asteroids and the largest one in the intermediate main belt with more than 5,000 members. The asteroid orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 5 months (1,603 days). Its orbit has an eccentricity of 0.17 and an inclination of 13 ° with respect to the ecliptic. It was first identified as at Simeiz Observatory in October 1914. The body's observation arc begins with its official discovery observation at Heidelberg in 1932. Naming This minor planet was named after the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lightcurve
In astronomy, a light curve is a graph of light intensity of a celestial object or region as a function of time, typically with the magnitude of light received on the y axis and with time on the x axis. The light is usually in a particular frequency interval or band. Light curves can be periodic, as in the case of eclipsing binaries, Cepheid variables, other periodic variables, and transiting extrasolar planets, or aperiodic, like the light curve of a nova, a cataclysmic variable star, a supernova or a microlensing event or binary as observed during occultation events. The study of the light curve, together with other observations, can yield considerable information about the physical process that produces it or constrain the physical theories about it. Variable stars Graphs of the apparent magnitude of a variable star over time are commonly used to visualise and analyse their behaviour. Although the categorisation of variable star types is increasingly done from their spe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eunomia Asteroid
The Eunomia or Eunomian family () is a large asteroid family of S-type asteroids named after the asteroid 15 Eunomia. It is the most prominent family in the intermediate asteroid belt and the 6th-largest family with nearly six thousand known members, or approximately 1.4% of all asteroids in the asteroid belt. Characteristics By far the largest member is 15 Eunomia, the largest of all the "stony" S-type asteroid, It is about 300 km across along its longest axis, has a 250 km mean radius, and lies close to the barycenter of the family. Eunomia has been estimated to contain about 70–75% of the matter from the original parent body. This had a mean diameter of about 280 km and was disrupted by the catastrophic impact that created the family. It is likely that the parent body was at least partly differentiated, because the surface of Eunomia and spectra of the smaller family members show some variation. This notwithstanding, other studies have indicated that the body ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gaius Marius
Gaius Marius (; – 13 January 86 BC) was a Roman general and statesman. Victor of the Cimbric and Jugurthine wars, he held the office of consul an unprecedented seven times during his career. He was also noted for his important reforms of Roman armies. He set the precedent for the shift from the militia levies of the middle Republic to the professional soldiery of the late Republic; he also improved the '' pilum'', a javelin, and made large-scale changes to the logistical structure of the Roman army. Rising from a well-off provincial Italian family in Arpinum, Marius acquired his initial military experience serving with Scipio Aemilianus at the Siege of Numantia in 134 BC. He won election as tribune of the plebs in 119 BC and passed a law limiting aristocratic interference in elections. Barely elected praetor in 115 BC, he next became the governor of Further Spain where he campaigned against bandits. On his return from Spain he married Julia, the aunt of J ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ambrones
The Ambrones ( grc, Ἄμβρωνες) were an ancient tribe mentioned by Roman authors. They are generally believed to have been a Germanic tribe from Jutland. In the late 2nd century BC, along with the fellow Cimbri and Teutons, the Ambrones migrated from their original homes and invaded the Roman Republic, winning a spectacular victory at the Battle of Arausio in 105 BC. The Ambrones and the Teutons, led by Teutobod, were eventually defeated at the Battle of Aquae Sextiae in 102 BC. Name The origin of the name ''Ambrones'' poses a great difficulty in explanation, since the root ''Ambr''- and its variants are found in many areas of the European continent: the Ombrones of the upper Vistula, the *Ymbre (dat. ''Ymbrum''), a tribe mentioned in the ''Widsith'', the islands of Amrum (older ''Ambrum'') and Imbria (modern Fehmarn), the river names Ammer, Amper, and Emmer, the region of Ammerland, the town of Emmerich, as well as the Italic Umbri (or ''Ombrii'') and the Greek person ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Teutons
The Teutons ( la, Teutones, , grc, Τεύτονες) were an ancient northern European tribe mentioned by Roman authors. The Teutons are best known for their participation, together with the Cimbri and other groups, in the Cimbrian War with the Roman Republic in the late second century BC. Julius Caesar described them as a Germanic people, a term he applied to all northern peoples located east of the Rhine, and later Roman authors followed him. On one hand, there is no direct evidence that they spoke a Germanic language, and evidence such as their name, and the names of their rulers, indicates at least a strong influence from Celtic languages. On the other hand the indications that classical authors gave about the homeland of the Teutones is considered by many scholars to show that they lived in an area associated with early Germanic languages, and not Celtic languages. Name The ethnonym is attested in Latin as ''Teutonēs'' or ''Teutoni'' (plural) or, more rarely, as ''Teut ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Proto-Germanic
Proto-Germanic (abbreviated PGmc; also called Common Germanic) is the reconstructed proto-language of the Germanic branch of the Indo-European languages. Proto-Germanic eventually developed from pre-Proto-Germanic into three Germanic branches during the fifth century BC to fifth century AD: West Germanic, East Germanic and North Germanic, which however remained in contact over a considerable time, especially the Ingvaeonic languages (including English), which arose from West Germanic dialects and remained in continued contact with North Germanic. A defining feature of Proto-Germanic is the completion of the process described by Grimm's law, a set of sound changes that occurred between its status as a dialect of Proto-Indo-European and its gradual divergence into a separate language. As it is probable that the development of this sound shift spanned a considerable time (several centuries), Proto-Germanic cannot adequately be reconstructed as a simple node in a tree model but ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minor Planet
According to the International Astronomical Union (IAU), a minor planet is an astronomical object in direct orbit around the Sun that is exclusively classified as neither a planet nor a comet. Before 2006, the IAU officially used the term ''minor planet'', but that year's meeting reclassified minor planets and comets into dwarf planets and small Solar System bodies (SSSBs).Press release, IAU 2006 General Assembly: Result of the IAU Resolution votes International Astronomical Union, August 24, 2006. Accessed May 5, 2008. Minor planets include asteroids ( |
Observation Arc
In observational astronomy, the observation arc (or arc length) of a Solar System body is the time period between its earliest and latest observations, used for tracing the body's path. It is usually given in days or years. The term is mostly used in the discovery and tracking of asteroids and comets. Arc length has the greatest influence on the accuracy of an orbit. The number and spacing of intermediate observations has a lesser effect. Short arcs A very short arc leaves a high uncertainty parameter. The object might be in one of many different orbits, at many distances from Earth. In some cases, the initial arc was too short to determine if the object was in orbit around the Earth, or orbiting out in the asteroid belt. With a 1-day observation arc, was thought to be a trans-Neptunian dwarf planet, but is now known to be a 1 km main-belt asteroid. With an observation arc of 3 days, was thought to be a Mars-crossing asteroid that could be a threat to Earth, but was later ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Simeiz Observatory
Simeiz Observatory (also spelled Simeis or Simeïs) was an astronomy research observatory until the mid-1950s. It is located on Mount Koshka, Crimea, , by the town of Simeiz. Part of the Crimean Astrophysical Observatory, it is currently used for laser based studies of the orbits of satellites. The Minor Planet Center (MPC) credits Simeiz Observatory as the location where a total of 150 minor planets were discovered by astronomers Grigory Neujmin, Sergey Belyavsky, Vladimir Albitsky, Grigory Shajn, Nikolaj Ivanov, Pelageya Shajn, Praskov'ja Parchomenko, Alexander Deutsch and Evgenij Skvorcov. As of 2017, the discovery of the minor planet is directly credited to Simeiz Observatory by the MPC. History The Simeiz Observatory was founded by Russian amateur astronomer Nikolai Maltsov, who later became a honored member of the Russian Academy of Sciences and after whom asteroid 749 Malzovia was named. In 1900, he built a tower for refractor at his land plot near Simei ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Ecliptic
The ecliptic or ecliptic plane is the orbital plane of the Earth around the Sun. From the perspective of an observer on Earth, the Sun's movement around the celestial sphere over the course of a year traces out a path along the ecliptic against the background of stars. The ecliptic is an important reference plane and is the basis of the ecliptic coordinate system. Sun's apparent motion The ecliptic is the apparent path of the Sun throughout the course of a year. Because Earth takes one year to orbit the Sun, the apparent position of the Sun takes one year to make a complete circuit of the ecliptic. With slightly more than 365 days in one year, the Sun moves a little less than 1° eastward every day. This small difference in the Sun's position against the stars causes any particular spot on Earth's surface to catch up with (and stand directly north or south of) the Sun about four minutes later each day than it would if Earth did not orbit; a day on Earth is therefore 24 hours ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orbital Inclination
Orbital inclination measures the tilt of an object's orbit around a celestial body. It is expressed as the angle between a reference plane and the orbital plane or axis of direction of the orbiting object. For a satellite orbiting the Earth directly above the Equator, the plane of the satellite's orbit is the same as the Earth's equatorial plane, and the satellite's orbital inclination is 0°. The general case for a circular orbit is that it is tilted, spending half an orbit over the northern hemisphere and half over the southern. If the orbit swung between 20° north latitude and 20° south latitude, then its orbital inclination would be 20°. Orbits The inclination is one of the six orbital elements describing the shape and orientation of a celestial orbit. It is the angle between the orbital plane and the plane of reference, normally stated in degrees. For a satellite orbiting a planet, the plane of reference is usually the plane containing the planet's equator. For pla ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orbital Eccentricity
In astrodynamics, the orbital eccentricity of an astronomical object is a dimensionless parameter that determines the amount by which its orbit around another body deviates from a perfect circle. A value of 0 is a circular orbit, values between 0 and 1 form an elliptic orbit, 1 is a parabolic escape orbit (or capture orbit), and greater than 1 is a hyperbola. The term derives its name from the parameters of conic sections, as every Kepler orbit is a conic section. It is normally used for the isolated two-body problem, but extensions exist for objects following a rosette orbit through the Galaxy. Definition In a two-body problem with inverse-square-law force, every orbit is a Kepler orbit. The eccentricity of this Kepler orbit is a non-negative number that defines its shape. The eccentricity may take the following values: * circular orbit: ''e'' = 0 * elliptic orbit: 0 < ''e'' < 1 * [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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