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1062 Ljuba
1062 Ljuba, provisional designation , is a carbonaceous background asteroid from the outer regions of the asteroid belt, approximately in diameter. The asteroid was discovered on 11 October 1925, by Soviet–Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula. It was named after female paratrooper Ljuba Berlin, who died at an early age. The C-type asteroid has a longer-than average rotation period of 33.8 hours. Orbit and classification ''Ljuba'' is a non-family asteroid from the main belt's background population. 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 (1,902 days; semi-major axis of 3 AU). Its orbit has an eccentricity of 0.07 and an inclination of 6 ° with respect to the ecliptic. The asteroid was first observed as at Heidelberg Observatory in October 1904. The body's observation arc also begins at Heidelberg in February 1929, or 16 months after its officia ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Sergey Belyavsky
Sergey Ivanovich Belyavsky (russian: Серге́й Ива́нович Беля́вский; December 7, 1883 (Julian calendar: November 25) – October 13, 1953) was a Soviet/Russian astronomer and a discoverer of 36 numbered minor planets. His last name is also alternatively spelled Beljavskij (name under which the Minor Planet Center credits him) or Beljawskij. His first name is occasionally given as "Sergius". He was born in St. Petersburg and was a member of the Academy of Sciences of the Soviet Union. His field of work included astrophotometry, astrometry, and the study of variable stars. He died in Leningrad. He discovered the bright naked-eye comet C/1911 S3 (Beljawsky), also known according to the nomenclature of the time as "Comet 1911 IV" or "Comet 1911g". Belyavsky observed at Simeiz Observatory (Симеиз) in Crimea. Between 1937 and 1944, Belyavsky was the seventh director of the Pulkovo Observatory The Pulkovo Astronomical Observatory (russian: ... [...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] |
IRAS
The Infrared Astronomical Satellite (Dutch: ''Infrarood Astronomische Satelliet'') (IRAS) was the first space telescope to perform a survey of the entire night sky at infrared wavelengths. Launched on 25 January 1983, its mission lasted ten months. The telescope was a joint project of the United States (NASA), the Netherlands ( NIVR), and the United Kingdom ( SERC). Over 250,000 infrared sources were observed at 12, 25, 60, and 100 micrometer wavelengths. Support for the processing and analysis of data from IRAS was contributed from the Infrared Processing and Analysis Center at the California Institute of Technology. Currently, the Infrared Science Archive at IPAC holds the IRAS archive. The success of IRAS led to interest in the 1985 Infrared Telescope (IRT) mission on the Space Shuttle, and the planned Shuttle Infrared Telescope Facility which eventually transformed into the Space Infrared Telescope Facility, SIRTF, which in turn was developed into the Spitzer Space ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
List Of Slow Rotators (minor Planets)
This is a list of slow rotators—minor planets that have an exceptionally long rotation period. This period, typically given in hours, and sometimes called rotation rate or spin rate, is a fundamental standard physical property for minor planets. In recent years, the periods of many thousands of bodies have been obtained from photometric and, to a lesser extent, radiometric observations. The periods given in this list are sourced from the ''Light Curve Data Base'' (LCDB), which contains lightcurve data for more than 15,000 bodies. Most minor planets have rotation periods between 2 and 20 hours. , a group of approximately 650 bodies, typically measuring 1–20 kilometers in diameter, have periods of more than 100 hours or 4 days. Among the slowest rotators, there are currently 15 bodies with a period longer than 1000 hours. According to the Minor Planet Center, the sharp lower limit of approximately 2.2 hours is due to the fact that most smaller bodies are thought to be ru ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Laurent Bernasconi
This is a list of minor-planet discoverers credited by the Minor Planet Center with the discovery of one or several minor planets (such as near-Earth and main-belt asteroids, Jupiter trojans and distant objects). , the discovery of 612,011 numbered minor planets are credited to 1141 astronomers and 253 observatories, telescopes or surveys ''(see )''. On how a discovery is made, ''see observations of small Solar System bodies. For a description of the tables below, see ''. Discovering astronomers }, (bio-de) , align=left , M. Matsuyama , , - id="D. Matter" , align=left , Daniel Matter , 7 , 1957–pres. , , align=left , D. Matter; amateur, (bio-it) , align=left , D. Matter , , - id="A. Maury" , align=left , Alain Maury , 9 , 1958–pres. , , align=left , A. Maury; , align=left , A. Maury , , - id="D. Mayes" , align=left , Deronda Mayes , , 1957–pres. , , align=left , D. Mayes; inferred , align=left , D. Mayes , , - id="E. Mazzoni ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
René Roy (astronomer)
This is a list of minor-planet discoverers credited by the Minor Planet Center with the discovery of one or several minor planets (such as near-Earth and main-belt asteroids, Jupiter trojans and distant objects). , the discovery of 612,011 numbered minor planets are credited to 1141 astronomers and 253 observatories, telescopes or surveys ''(see )''. On how a discovery is made, ''see observations of small Solar System bodies. For a description of the tables below, see ''. Discovering astronomers }, (bio-de) , align=left , M. Matsuyama , , - id="D. Matter" , align=left , Daniel Matter , 7 , 1957–pres. , , align=left , D. Matter; amateur, (bio-it) , align=left , D. Matter , , - id="A. Maury" , align=left , Alain Maury , 9 , 1958–pres. , , align=left , A. Maury; , align=left , A. Maury , , - id="D. Mayes" , align=left , Deronda Mayes , , 1957–pres. , , align=left , D. Mayes; inferred , align=left , D. Mayes , , - id="E. Mazz ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Richard Binzel
Richard "Rick" P. Binzel (born 1958) is an American astronomer and professor of planetary sciences at the Massachusetts Institute of Technology (MIT). He is a discoverer of minor planets, photometrist and the inventor of the Torino Scale, a method for categorizing the impact hazard associated with near-Earth objects such as asteroids and comets. He is also a frequent trip leader for the MIT Alumni Association. Biography and honors Binzel was awarded the H. C. Urey Prize by the American Astronomical Society in 1991. He also was awarded a "MacVicar Faculty Fellowship" for teaching excellence at MIT in 1994. He is a co-investigator on the OSIRIS-REx mission. Binzel was on the "Planet Definition Committee" that developed the proposal to the International Astronomical Union's meeting in Prague in 2006 on whether Pluto should be considered a planet. Their proposal was revised during the meeting and Pluto is now considered a dwarf planet. However, Richard Binzel has strong feeling ... [...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 their spe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Magnitude (astronomy)
In astronomy, magnitude is a unitless measure of the brightness Brightness is an attribute of visual perception in which a source appears to be radiating or reflecting light. In other words, brightness is the perception elicited by the luminance of a visual target. The perception is not linear to luminance, ... of an astronomical object, object in a defined passband, often in the visible spectrum, 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 scale, 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[5] \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 defini ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Walter R
Walter may refer to: People * Walter (name), both a surname and a given name * Little Walter, American blues harmonica player Marion Walter Jacobs (1930–1968) * Gunther (wrestler), Austrian professional wrestler and trainer Walter Hahn (born 1987), who previously wrestled as "Walter" * Walter, standard author abbreviation for Thomas Walter (botanist) ( – 1789) Companies * American Chocolate, later called Walter, an American automobile manufactured from 1902 to 1906 * Walter Energy, a metallurgical coal producer for the global steel industry * Walter Aircraft Engines, Czech manufacturer of aero-engines Films and television * Walter (1982 film), ''Walter'' (1982 film), a British television drama film * Walter Vetrivel, a 1993 Tamil crime drama film * Walter (2014 film), ''Walter'' (2014 film), a British television crime drama * Walter (2015 film), ''Walter'' (2015 film), an American comedy-drama film * Walter (2020 film), ''Walter'' (2020 film), an Indian crime drama film * ''W ... [...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] |
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] |
