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46610 Bésixdouze
46610 Bésixdouze (), provisional designation , is a bright background asteroid from the inner regions of the asteroid belt, approximately 2 kilometers in diameter. It was discovered on 15 October 1993, by Japanese amateur astronomers Kin Endate and Kazuro Watanabe at the Kitami Observatory in eastern Hokkaidō, Japan. The asteroid was named after "B-612", home of ''The Little Prince''. Orbit and classification ''Bésixdouze'' is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner main-belt at a distance of 1.9–2.7 AU once every 3 years and 5 months (1,249 days; semi-major axis of 2.27 AU). Its orbit has an eccentricity of 0.18 and an inclination of 2 ° with respect to the ecliptic. The asteroid was first identified as at Crimea–Nauchnij in a single image taken in September 1986. Physical characteristics Diameter and albedo According to the survey carried out by the NEOWISE mission of NASA's Wide-field Inf ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kin Endate
is a Japanese amateur astronomer who has discovered hundreds of asteroids, most of them in collaboration with Kazuro Watanabe, placing him among the most prolific discoverers of minor planets. Career in astronomy Kin Endate was born in Iwaizumi in Iwate Prefecture and went to Hokkaido Designers School to study photography. He began taking astrophotos in high school, but did not begin serious asteroid observations until 1986. His notable discoveries include the minor planets (5648) 1990 VU1 and 6500 Kodaira, a Jupiter trojan and the Mars-crosser, respectively. He also recorded the first known precovery images of Comet Shoemaker-Levy 9 with his private diameter telescope on March 15, 1993, ten days before the official discovery of the comet. Kin, who was looking specifically for asteroids, did not know of the comet in his images until after the official discovery. [...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] |
B612 Foundation
The B612 Foundation is a private nonprofit foundation headquartered in Mill Valley, California, United States, dedicated to planetary science and planetary defense against asteroids and other near-Earth object (NEO) impacts. It is led mainly by scientists, former astronauts and engineers from the Institute for Advanced Study, Southwest Research Institute, Stanford University, NASA and the space industry. As a non-governmental organization it has conducted two lines of related research to help detect NEOs that could one day strike the Earth, and find the technological means to divert their path to avoid such collisions. It also assisted the Association of Space Explorers in helping the United Nations establish the International Asteroid Warning Network, as well as a Space Missions Planning Advisory Group to provide oversight on proposed asteroid deflection missions. In 2012, the foundation announced it would design and build a privately financed asteroid-finding space obs ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
2578 Saint-Exupéry
2578 Saint-Exupéry, provisional designation , is an Eoan asteroid from the outer region of the asteroid belt, approximately 17 kilometers in diameter. It was discovered by Russian astronomer Tamara Smirnova at the Crimean Astrophysical Observatory in Nauchnyj on 2 November 1975, and named after French aviator and writer Antoine de Saint-Exupéry. Classification and orbit ''Saint-Exupéry'' is a member the Eos family (), the largest asteroid family of the outer main belt consisting of nearly 10,000 known members. The asteroid orbits the Sun at a distance of 2.7–3.3 AU once every 5 years and 2 months (1,900 days). Its orbit has an eccentricity of 0.10 and an inclination of 11 ° with respect to the ecliptic. The asteroid's was first identified as at McDonald Observatory in Texas. One month later, it was also observed at the Palomar Observatory in May 1952. Its observation arc begins by 23 years prior to its official discovery observation at Nauchnyj. Physical cha ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minor Planet Circulars
The Minor Planet Center (MPC) is the official body for observing and reporting on minor planets under the auspices of the International Astronomical Union (IAU). Founded in 1947, it operates at the Smithsonian Astrophysical Observatory. Function The Minor Planet Center is the official worldwide organization in charge of collecting observational data for minor planets (such as asteroids), calculating their orbits and publishing this information via the '' Minor Planet Circulars''. Under the auspices of the International Astronomical Union (IAU), it operates at the Smithsonian Astrophysical Observatory, which is part of the Center for Astrophysics along with the Harvard College Observatory. The MPC runs a number of free online services for observers to assist them in observing minor planets and comets. The complete catalogue of minor planet orbits (sometimes referred to as the "Minor Planet Catalogue") may also be freely downloaded. In addition to astrometric data, the MPC collect ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Minor Planet Center
The Minor Planet Center (MPC) is the official body for observing and reporting on minor planets under the auspices of the International Astronomical Union (IAU). Founded in 1947, it operates at the Smithsonian Astrophysical Observatory. Function The Minor Planet Center is the official worldwide organization in charge of collecting observational data for minor planets (such as asteroids), calculating their orbits and publishing this information via the '' Minor Planet Circulars''. Under the auspices of the International Astronomical Union (IAU), it operates at the Smithsonian Astrophysical Observatory, which is part of the Center for Astrophysics along with the Harvard College Observatory. The MPC runs a number of free online services for observers to assist them in observing minor planets and comets. The complete catalogue of minor planet orbits (sometimes referred to as the "Minor Planet Catalogue") may also be freely downloaded. In addition to astrometric data, the MPC collect ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Hexadecimal
In mathematics and computing, the hexadecimal (also base-16 or simply hex) numeral system is a positional numeral system that represents numbers using a radix (base) of 16. Unlike the decimal system representing numbers using 10 symbols, hexadecimal uses 16 distinct symbols, most often the symbols "0"–"9" to represent values 0 to 9, and "A"–"F" (or alternatively "a"–"f") to represent values from 10 to 15. Software developers and system designers widely use hexadecimal numbers because they provide a human-friendly representation of binary-coded values. Each hexadecimal digit represents four bits (binary digits), also known as a nibble (or nybble). For example, an 8-bit byte can have values ranging from 00000000 to 11111111 in binary form, which can be conveniently represented as 00 to FF in hexadecimal. In mathematics, a subscript is typically used to specify the base. For example, the decimal value would be expressed in hexadecimal as . In programming, a number of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Jiří Grygar
Jiří Grygar (; March 17, 1936, in Heinersdorf, Germany, now Dziewiętlice, Poland) is a Czech astronomer, popularizer of science and Kalinga Prize (1996) laureate. Career After studying physics at the Masaryk University in Brno and astronomy at the Charles University in Prague he joined the Astronomical Institute of the Academy of Sciences, Department of Stellar Astronomy in Ondřejov. Twenty years later he moved to the Institute of Physics, Low Temperature Physics Department at Řež, where he remained for more than ten years. Shortly after the Velvet Revolution he joined the High Energy Physics Department at the same institution. From 1992 to 1998, Grygar chaired the Czech Astronomical Society. He also chaired the Czech Television Council and the Science and Philosophy section of the European Culture Club. He is member of editorial boards of the periodicals ''Říše hvězd'', '' Vesmír'', ''Universum'' and ''Omega''. Grygar holds a PhD in astrophysics. His papers focus ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Rotation Period
The rotation period of a celestial object (e.g., star, gas giant, planet, moon, asteroid) may refer to its sidereal rotation period, i.e. the time that the object takes to complete a single revolution around its axis of rotation relative to the background stars, measured in sidereal time. The other type of commonly used rotation period is the object's synodic rotation period (or ''solar day''), measured in solar time, which may differ by a fraction of a rotation or more than one rotation to accommodate the portion of the object's orbital period during one day. Measuring rotation For solid objects, such as rocky planets and asteroids, the rotation period is a single value. For gaseous or fluid bodies, such as stars and gas giants, the period of rotation varies from the object's equator to its pole due to a phenomenon called differential rotation. Typically, the stated rotation period for a gas giant (such as Jupiter, Saturn, Uranus, Neptune) is its internal rotation period, as d ... [...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] |
S-type Asteroid
S-type asteroids are asteroids with a spectral type that is indicative of a siliceous (i.e. stony) mineralogical composition, hence the name. They have relatively high density. Approximately 17% of asteroids are of this type, making it the second most common after the carbonaceous C-type. Characteristics S-type asteroids, with an astronomical albedo of typically 0.20, are moderately bright and consist mainly of iron- and magnesium-silicates. They are dominant in the inner part of the asteroid belt within 2.2 AU, common in the central belt within about 3 AU, but become rare farther out. The largest are 3 Juno (about 240–250 km across) and 15 Eunomia (230 km), with other large S-types being 29 Amphitrite, 532 Herculina and 7 Iris. These largest S-types are visible in 10x50 binoculars at most oppositions; the brightest, 7 Iris, can occasionally become brighter than +7.0, which is a higher magnitude than any asteroid except the unusually reflective 4 Vesta. T ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astronomical Albedo
Albedo (; ) is the measure of the diffuse reflection of solar radiation out of the total solar radiation and measured on a scale from 0, corresponding to a black body that absorbs all incident radiation, to 1, corresponding to a body that reflects all incident radiation. Surface albedo is defined as the ratio of radiosity ''J''e to the irradiance ''E''e (flux per unit area) received by a surface. The proportion reflected is not only determined by properties of the surface itself, but also by the spectral and angular distribution of solar radiation reaching the Earth's surface. These factors vary with atmospheric composition, geographic location, and time (see position of the Sun). While bi-hemispherical reflectance is calculated for a single angle of incidence (i.e., for a given position of the Sun), albedo is the directional integration of reflectance over all solar angles in a given period. The temporal resolution may range from seconds (as obtained from flux measurements) to ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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