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2429 Schürer
2429 Schürer, provisional designation , is a Maria asteroid from the central region of the asteroid belt, approximately in diameter. It was discovered on 12 October 1977, by Swiss astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland, and later named after Swiss astronomer Max Schürer. The likely elongated S-type asteroid has a rotation period of 6.6 hours. Orbit and classification ''Schürer'' is a member of the Maria family (506), a large family of stony asteroids with nearly 3000 known members, named after asteroid 170 Maria. The family is old, about years, and located near the 3:1 resonant region with Jupiter that supplies near-Earth objects to the inner Solar System. It is estimated that every 100 million years, about 37 to 75 Maria asteroids larger than 1 kilometer become such near-Earth objects. It orbits the Sun in the central main-belt at a distance of 2.3–2.8 AU once every 4 years and 1 month (1,507 days; semi-major axis of 2.57& ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Paul Wild (Swiss Astronomer)
Paul Wild (; 5 October 1925 – 2 July 2014) was a Swiss astronomer An astronomer is a scientist in the field of astronomy who focuses their studies on a specific question or field outside the scope of Earth. They observe astronomical objects such as stars, planets, natural satellite, moons, comets and galaxy, g ... and director of the Astronomical Institute of the University of Bern, who discovered numerous comets, asteroids and supernovae. Biography Wild was born on 5 October 1925 in the village of Wädenswil near Zürich, Switzerland. From 1944 through 1950, he studied mathematics and physics at the ETH Zurich. Thereafter, he worked at the California Institute of Technology where he researched galaxies and supernovas under the leadership of countryman Fritz Zwicky from 1951 through 1955. At the Zimmerwald Observatory, near Bern, Wild made his first cometary discovery C/1957 U1 (1957 IX) on 2 October 1957. The parabolic comet was later named "Latyshev-Wild–Robert Burn ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Orbital Resonance
In celestial mechanics, orbital resonance occurs when orbiting bodies exert regular, periodic gravitational influence on each other, usually because their orbital periods are related by a ratio of small integers. Most commonly, this relationship is found between a pair of objects (binary resonance). The physical principle behind orbital resonance is similar in concept to pushing a child on a swing, whereby the orbit and the swing both have a natural frequency, and the body doing the "pushing" will act in periodic repetition to have a cumulative effect on the motion. Orbital resonances greatly enhance the mutual gravitational influence of the bodies (i.e., their ability to alter or constrain each other's orbits). In most cases, this results in an ''unstable'' interaction, in which the bodies exchange momentum and shift orbits until the resonance no longer exists. Under some circumstances, a resonant system can be self-correcting and thus stable. Examples are the 1:2:4 resonance ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1748 Mauderli
1748 Mauderli, provisional designation , is a dark and very reddish Hildian asteroid from the outermost region of the asteroid belt, approximately 45 kilometers in diameter. It was discovered on 7 September 1966, by astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland, and was later named after Swiss astronomer Sigmund Mauderli. Orbit and classification ''Mauderli'' is a member of the Hilda family of asteroids which stay in a 3:2 resonance with the gas giant Jupiter. Among the Hilda family, it is one of its members with the highest amplitude of libration relative to the stable periodic orbit. The asteroid orbits the Sun in the outermost main-belt at a distance of 3.1–4.8 AU once every 7 years and 10 months (2,857 days). Its orbit has an eccentricity of 0.22 and an inclination of 3 ° with respect to the ecliptic. ''Mauderli'' was first identified as at Heidelberg Observatory in 1922, extending the body's observation arc by 44 years prior to its o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1775 Zimmerwald
1775 Zimmerwald, provisional designation , is a stony Eunomian asteroid and slow rotator from the middle region of the asteroid belt, approximately 10 kilometers in diameter. It was discovered on 13 May 1969, by Swiss astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland. It is named for the village of Zimmerwald, where the discovering observatory is located. Orbit and classification ''Zimmerwald'' is a member of the Eunomia family, a large group of mostly stony S-type asteroids and the most prominent family in the intermediate main-belt, which is located between two prominent Kirkwood gaps. It orbits the Sun in the central main-belt at a distance of 2.1–3.1 AU once every 4 years and 2 months (1,533 days). Its orbit has an eccentricity of 0.19 and an inclination of 13 ° with respect to the ecliptic. The first precovery of ''Zimmerwald'' was taken at Palomar Observatory in 1949, extending the body's observation arc by 20 years prior to its official disc ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
University Of Bern
The University of Bern (german: Universität Bern, french: Université de Berne, la, Universitas Bernensis) is a university in the Switzerland, Swiss capital of Bern and was founded in 1834. It is regulated and financed by the Canton of Bern. It is a comprehensive university offering a broad choice of courses and programs in eight faculty (division), faculties and some 150 institutes. With around 18,576 students, the University of Bern is the third largest university in Switzerland. Organization The University of Bern operates at three levels: university, faculties and institutes. Other organizational units include interfaculty and general university units. The university's highest governing body is the Senate, which is responsible for issuing statutes, rules and regulations. Directly answerable to the Senate is the University Board of Directors, the governing body for university management and coordination. The board comprises the rector, the vice-rectors and the administrati ... [...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 ( |
Heidelberg Observatory
Heidelberg (; Palatine German: '''') is a city in the German state of Baden-Württemberg, situated on the river Neckar in south-west Germany. As of the 2016 census, its population was 159,914, of which roughly a quarter consisted of students. Located about south of Frankfurt, Heidelberg is the fifth-largest city in Baden-Württemberg. Heidelberg is part of the densely populated Rhine-Neckar Metropolitan Region. Heidelberg University, founded in 1386, is Germany's oldest and one of Europe's most reputable universities. Heidelberg is a scientific hub in Germany and home to several internationally renowned research facilities adjacent to its university, including the European Molecular Biology Laboratory and four Max Planck Institutes. The city has also been a hub for the arts, especially literature, throughout the centuries, and it was designated a "City of Literature" by the UNESCO Creative Cities Network. Heidelberg was a seat of government of the former Electorate of the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Precovery
In astronomy, precovery (short for pre-discovery recovery) is the process of finding the image of an object in images or photographic plates predating its discovery, typically for the purpose of calculating a more accurate orbit. This happens most often with minor planets, but sometimes a comet, a dwarf planet, a natural satellite, or a star is found in old archived images; even exoplanet precovery observations have been obtained. "Precovery" refers to a pre-discovery image; "recovery" refers to imaging of a body which was lost to our view (as behind the Sun), but is now visible again ''(also see lost minor planet and lost comet)''. Orbit determination requires measuring an object's position on multiple occasions. The longer the interval between observations, the more accurately the orbit can be calculated; however, for a newly discovered object, only a few days' or weeks' worth of measured positions may be available, sufficient only for a preliminary (imprecise) orbit calculatio ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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] |
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] |
