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1309 Hyperborea
1309 Hyperborea is a carbonaceous background asteroid from the outermost regions of the asteroid belt, approximately 57 kilometers in diameter. It was discovered on 11 October 1931, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula, and given the provisional designation . The asteroid was named after Hyperborea, the northern homeland of a Greek mythical race of giants. Orbit and classification ''Hyperborea'' is a non- family asteroid of the main belt's background population. It orbits the Sun in the outermost asteroid belt at a distance of 2.7–3.7 AU once every 5 years and 9 months (2,098 days; semi-major axis of 3.21 AU). Its orbit has an eccentricity of 0.15 and an inclination of 10 ° with respect to the ecliptic. The body's observation arc begins at Heidelberg Observatory with its first observations as in September 1919, or 12 years prior to its official discovery observation at Simeiz. Physical characteristi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Grigory Neujmin
Grigory Nikolayevich Neujmin (russian: Григорий Николаевич Неуймин; – 17 December 1946) was a Georgian–Russian astronomer, native of Tbilisi in Georgia, and a discoverer of numerous minor planets as well as 6 periodic and a hyperbolic comet at the Pulkovo and Simeiz Observatories during the first half of the 20th century. Discoveries The Minor Planet Center credits his discoveries under the name "G. N. Neujmin", and his surname appears this way in the literature. However, the modern English transliteration of his name would be Neuymin. Neujmin is credited with the discovery of 74 asteroids, and notably 951 Gaspra and 762 Pulcova. He also discovered and co-discovered 6 Jupiter-family comets, namely 25D/Neujmin, 28P/Neujmin, 42P/Neujmin, 57P/du Toit-Neujmin-Delporte (including fragment A) and 58P/Jackson–Neujmin, as well as C/1914 M1 (Neujmin), a hyperbolic comet. Awards and honors He received the Order of the Red Banner of Labour on 1 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Semi-major 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 cen ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Magnitude (astronomy)
In astronomy, magnitude is a unitless measure of the brightness of an object in a defined passband, often in the visible or infrared spectrum, but sometimes across all wavelengths. An imprecise but systematic determination of the magnitude of objects was introduced in ancient times by Hipparchus. The scale is logarithmic and defined such that a magnitude 1 star is exactly 100 times brighter than a magnitude 6 star. Thus each step of one magnitude is \sqrt \approx 2.512 times brighter than the magnitude 1 higher. The brighter an object appears, the lower the value of its magnitude, with the brightest objects reaching negative values. Astronomers use two different definitions of magnitude: apparent magnitude and absolute magnitude. The ''apparent'' magnitude () is the brightness of an object as it appears in the night sky from Earth. Apparent magnitude depends on an object's intrinsic luminosity, its distance, and the extinction reducing its brightness. The ''absolute'' magnitu ... [...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 Poles of astronomical bodies, 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 in ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
LCDB Quality Code
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 t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Rozhen Observatory
Rozhen Observatory ( bg, Национална астрономическа обсерватория - Рожен, ''НАО-Рожен''; en, National Astronomical Observatory - Rozhen, ''NAO-Rozhen''), also known as the Bulgarian National Astronomical Observatory, is an astronomical observatory, located in the Smolyan Province, 90 kilometers south of the city of Plovdiv, Bulgaria. The nearest town, Chepelare, is 15 kilometers away. The observatory is owned and operated by the Institute of Astronomy of the Bulgarian Academy of Sciences (BAS). It was officially opened on 13 March 1981, almost 20 years after Bogomil Kovachev – a professor of astronomy at BAS, known as its founder – had started working towards that goal. The Observatory is the largest in Southeastern Europe and has an active team of about 50 astronomers. It is the principal center for astronomical research in Bulgaria. The minor planet 6267 Rozhen, was discovered at, and named after the observatory. With its to ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Oakley Southern Sky Observatory
This is a list of observatory codes (IAU codes or MPC codes) published by the 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 .... For a detailed description, ''see observations of small Solar System bodies''. List References * {{DEFAULTSORT:Observatory codes * Astronomy-related lists Technology-related lists ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Pierre Antonini
Pierre Antonini is a retired French mathematics professor and amateur astronomer who has discovered several minor planets and two supernovae at his private Observatoire de Bédoin (Bedoin Observatory; observatory code: 132) located at Bédoin, southeastern France. For many of his discoveries he used a 16-cm telescope or a 30-cm telescope. He is a prolific discoverer of asteroids. The Minor Planet Center (MPC) credits him with the discovery of 35 numbered minor planets between 1997–1999. As of March 2016, the MPC ranks him 204th in the all-time, top-astronomer chart by number of discovered bodies. Antonini is also credited with the discovery of the supernovae and . In January 2004, he co-discovered S/2003 (1089) 1, a minor planet moon orbiting the main-belt asteroid 1089 Tama. The 7-kilometer sized main-belt asteroid 12580 Antonini, discovered by Laurent Bernasconi in 1999, was named in his honour. List of discovered minor planets See also * International Astron ... [...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 t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Pan-STARRS
The Panoramic Survey Telescope and Rapid Response System (Pan-STARRS1; obs. code: F51 and Pan-STARRS2 obs. code: F52) located at Haleakala Observatory, Hawaii, US, consists of astronomical cameras, telescopes and a computing facility that is surveying the sky for moving or variable objects on a continual basis, and also producing accurate astrometry and photometry of already-detected objects. In January 2019 the second Pan-STARRS data release was announced. At 1.6 petabytes, it is the largest volume of astronomical data ever released. Description The Pan-STARRS Project is a collaboration between the University of Hawaii Institute for Astronomy, MIT Lincoln Laboratory, Maui High Performance Computing Center and Science Applications International Corporation. Telescope construction was funded by the U.S. Air Force. By detecting differences from previous observations of the same areas of the sky, Pan-STARRS is discovering many new asteroids, comets, variable stars, s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 ... [...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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
