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6498 Ko
6498 Ko, provisional designation , is a stony Flora asteroid and exceptionally slow rotator from the inner regions of the asteroid belt, approximately 4 kilometers in diameter. The asteroid was discovered on 26 October 1992, by Japanese amateur astronomers Kin Endate and Kazuro Watanabe at Kitami Observatory on eastern Hokkaidō, Japan. It was named for Japanese scientist Ko Nagasawa. Orbit and classification ''Ko'' is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. 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 (1,258 days). Its orbit has an eccentricity of 0.17 and an inclination of 8 ° with respect to the ecliptic. A first precovery was taken at Palomar Observatory in 1954, extending the asteroid's observation arc by 38 years prior to its discovery. Minor-planet close approaches Although ''Ko'' does not cross the orbit of any planet, it does make close appro ... [...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] |
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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Astronomical Albedo
Albedo (; ) is the measure of the diffuse reflection of sunlight, 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 (radiometry), 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 ob ... [...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] |
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] |
Ondřejov Observatory
The Ondřejov Observatory (; cs, Observatoř Ondřejov) is the principal observatory of the Astronomical Institute () of the Academy of Sciences of the Czech Republic. It is located near the village of Ondřejov, southeast of Prague, Czech Republic. It has a wide telescope, which is the largest in the Czech Republic. History The facility was constructed in 1898, by Czech amateur astronomer and entrepreneur Josef Jan Frič as a private observatory. On 28 October 1928, he donated the facility to the Czechoslovak state to celebrate the tenth anniversary of its independence. The observatory, located at an altitude of , away from the air and light pollution of urban Prague, was administered by Charles University until the founding of the Czechoslovak Academy of Sciences in 1953, which from then on operated it as part of its Astronomical Institute in conjunction with other Czechoslovak observatories. In 1967, a telescope measuring in width was added to the observatory, which at ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Petr Pravec
Petr Pravec (born September 17, 1967) is a Czech astronomer and a discoverer of minor planets, born in Třinec, Czech Republic. Pravec is a prolific discoverer of binary asteroids, expert in photometric observations and rotational lightcurves at Ondřejov Observatory. He is credited by the Minor Planet Center with the discovery and co-discovery of 350 numbered minor planets, and is leading the effort of a large consortium of stations called "BinAst" to look for multiplicity in the near-Earth objects and inner main-belt populations. He is a member of the ''Academy of Sciences of the Czech Republic''. The main-belt asteroid 4790 Petrpravec 4790 Petrpravec ( ''prov. designation'': ) is a carbonaceous background asteroid from the central regions of the asteroid belt, approximately in diameter. It was discovered on 9 August 1988, by American astronomer Eleanor Helin at the Palomar ..., discovered by Eleanor Helin in 1988, is named after him. The official naming citation ... [...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] |
3 Juno
3 Juno is a large asteroid in the asteroid belt. Juno was the third asteroid discovered, in 1804, by German astronomer Karl Ludwig Harding, Karl Harding. It is one of the List of exceptional asteroids, twenty largest asteroids and one of the two largest stony (S-type asteroid, S-type) asteroids, along with 15 Eunomia. It is estimated to contain 1% of the total mass of the asteroid belt. History Discovery Juno was discovered on 1 September 1804, by Karl Ludwig Harding. It was the third asteroid found, but was initially considered to be a planet; it was reclassified as an asteroid and minor planet during the 1850s. Name and symbol Juno is named after the mythological Juno (mythology), Juno, the highest Roman goddess. The adjectival form is Junonian (from Latin ''jūnōnius''), with the historical final ''n'' of the name (still seen in the French form, ''Junon'') reappearing, analogous to Pluto ~ Plutonian. 'Juno' is the international name for the asteroid, subject to loca ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
29 Amphitrite
Amphitrite (minor planet designation: 29 Amphitrite) is one of the largest S-type asteroids, approximately in diameter, and probably fifth largest after Eunomia, Juno, Iris and Herculina. Discovery Amphitrite was discovered by Albert Marth on 1 March 1854, at the private South Villa Observatory, in Regent's Park, London. It was Marth's only asteroid discovery. Its name was chosen by George Bishop, the owner of the observatory, who named it after Amphitrite, a sea goddess in Greek mythology. Characteristics Amphitrite's orbit is less eccentric and inclined than those of its larger cousins; indeed, it is the most circular of any asteroid discovered up to that point. As a consequence, it never becomes as bright as Iris or Hebe, especially as it is much further from the Sun than those asteroids. It can reach magnitudes of around +8.6 at a favorable opposition, but usually is around the binocular limit of +9.5. In 2007, James Baer and Steven R. Chesley estimated Amphitri ... [...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] |
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