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2055 Dvořák
2055 Dvořák ( or ), provisional designation , is an eccentric asteroid and sizable Mars-crosser from the innermost regions of the asteroid belt, approximately 8 kilometers in diameter. It was discovered on 19 February 1974, by Czech astronomer Luboš Kohoutek at the Bergedorf Observatory in Hamburg, Germany. It was named after Czech composer Antonín Dvořák. Classification and orbit ''Dvořák'' is a Mars-crossing asteroid, as it crosses the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.6–3.0 AU once every 3 years and 6 months (1,283 days). Its orbit has an eccentricity of 0.31 and an inclination of 21 ° with respect to the ecliptic. The body's observation arc begins with its official discovery observation at Bergedorf in 1974. Physical characteristics Lightcurves In July 2013, two rotational lightcurves of ''Dvořák'' were obtained from photometric observations by Julian Oey at the Blue Mountain Observatory (), Australia, and by a col ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Luboš Kohoutek
Luboš Kohoutek (, born 29 January 1935) is a Czech astronomer and a discoverer of minor planets and comets, including Comet Kohoutek which was visible to the naked eye in 1973. He also discovered a large number of planetary nebulae. Biography Kohoutek was born in 1935 to Hynek and Jarmila Kohoutek. His brother was the Czech composer Ctirad Kohoutek. Kohoutek has been interested in astronomy since high school. He studied physics and astronomy at universities in Brno and Prague (finished 1958). Then he started to work in the Astronomical Institute of Czechoslovak Academy of Sciences, where he published a well-cited catalogue (''Catalogue of Galactic Planetary Nebulae'', 1967). Kohoutek obtained a long term position at the Bergedorf Observatory in Hamburg. After the Soviet occupation of Czechoslovakia (1968) he decided to stay in West Germany (1970). His discoveries in the 1970s made him well-known in the media. In later years Kohoutek worked in observatories in Spain and Chile, w ... [...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] |
Bedřich Smetana
Bedřich Smetana ( , ; 2 March 1824 – 12 May 1884) was a Czech composer who pioneered the development of a musical style that became closely identified with his people's aspirations to a cultural and political "revival." He has been regarded in his homeland as the father of Czech music. Internationally he is best known for his 1866 opera ''The Bartered Bride'' and for the symphonic cycle ''Má vlast'' ("My Fatherland"), which portrays the history, legends and landscape of the composer's native Bohemia. It contains the famous symphonic poem "Vltava", also popularly known by its German name "Die Moldau" (in English, "The Moldau"). Smetana was naturally gifted as a composer, and gave his first public performance at the age of 6. After conventional schooling, he studied music under Josef Proksch in Prague. His first nationalistic music was written during the 1848 Prague uprising, in which he briefly participated. After failing to establish his career in Prague, he left for Sweden ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Antonin Dvořák
Antonin may refer to: People * Antonin (name) Places ;Poland * Antonin, Jarocin County, Greater Poland Voivodeship * Antonin, Kalisz County, Greater Poland Voivodeship * Antonin, Oborniki County, Greater Poland Voivodeship * Antonin, Ostrów Wielkopolski County, Greater Poland Voivodeship * Antonin, Poznań County, Greater Poland Voivodeship * Antonin, Środa Wielkopolska County, Greater Poland Voivodeship * Antonin, Sieradz County, Łódź Voivodeship * Antonin, Zduńska Wola County, Łódź Voivodeship * Antonin, Masovian Voivodeship * Antonin, Podlaskie Voivodeship * Antonin, Pomeranian Voivodeship * Antonin, part of Nowe Miasto, Poznań, Greater Poland Voivodeship See also *Antolin (name) * Antonina (other) * Antonini (other) *Antonino (other) * Antoniny (other) * Antoninus (other) *Antoniu *Antonen Antonen is a Finnish surname. Notable people with the surname include: *Joose Antonen (born 1995), Finnish ice hockey ... [...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 ( |
Wide-field Infrared Survey Explorer
Wide-field Infrared Survey Explorer (WISE, observatory code C51, Explorer 92 and SMEX-6) is a NASA infrared astronomy space telescope in the Explorers Program. It was launched in December 2009, and placed in hibernation mode in February 2011, before being re-activated in 2013 and renamed the Near-Earth Object Wide-field Infrared Survey Explorer (NEOWISE). WISE discovered thousands of minor planets and numerous star clusters. Its observations also supported the discovery of the first Y-type brown dwarf and Earth trojan asteroid. WISE performed an all-sky astronomical survey with images in 3.4, 4.6, 12 and 22 μm wavelength range bands, over ten months using a diameter infrared telescope in Earth orbit. After its solid hydrogen coolant depleted, a four-month mission extension called NEOWISE was conducted to search for near-Earth objects (NEO) such as comets and asteroids using its remaining capability. The WISE All-Sky (WISEA) data, including processed images, source cat ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Akari (satellite)
Akari (ASTRO-F) was an infrared astronomy satellite developed by Japan Aerospace Exploration Agency, in cooperation with institutes of Europe and Korea. It was launched on 21 February 2006, at 21:28 UTC (06:28, 22 February JST) by M-V rocket into Earth sun-synchronous orbit. After its launch it was named ''Akari'' (明かり), which means ''light'' in Japanese. Earlier on, the project was known as IRIS (InfraRed Imaging Surveyor). Its primary mission was to survey the entire sky in near-, mid- and far-infrared, through its aperture telescope. Technical design Its designed lifespan, of far- and mid-infrared sensors, was 550 days, limited by its liquid helium coolant. Its telescope mirror was made of silicon carbide to save weight. The budget for the satellite was ¥13,4 billion (~). History By mid-August 2006, Akari finished around 50 percent of the all sky survey. By early November 2006, first (phase-1) all-sky survey finished. Second (phase-2) all-sky survey started ... [...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] |
Absolute Magnitude
Absolute magnitude () is a measure of the luminosity of a celestial object on an inverse Logarithmic scale, logarithmic Magnitude (astronomy), astronomical magnitude scale. An object's absolute magnitude is defined to be equal to the apparent magnitude that the object would have if it were viewed from a distance of exactly , without Extinction (astronomy), extinction (or dimming) of its light due to absorption by Interstellar medium, interstellar matter and cosmic dust. By hypothetically placing all objects at a standard reference distance from the observer, their luminosities can be directly compared among each other on a magnitude scale. As with all astronomical magnitude (astronomy), magnitudes, the absolute magnitude can be specified for different wavelength ranges corresponding to specified Filter (optics), filter bands or passbands; for stars a commonly quoted absolute magnitude is the absolute visual magnitude, which uses the visual (V) band of the spectrum (in the UBV phot ... [...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] |
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] |
