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Vulpecula (Chinese Astronomy)
The modern constellation Vulpecula lies across one of the quadrants symbolized by the Black Tortoise of the North (北方玄武, ''Běi Fāng Xuán Wǔ''), and Three Enclosures (三垣, ''Sān Yuán''), that divide the sky in traditional Chinese uranography. The name of the western constellation in modern Chinese is 狐狸座 (''hú li zuò''), meaning "the fox constellation". Stars The map of Chinese constellation in constellation Vulpecula area consists of : See also *Traditional Chinese star names *Chinese constellations Traditional Chinese astronomy has a system of dividing the celestial sphere into asterisms or constellations, known as "officials" (Chinese ''xīng guān''). The Chinese asterisms are generally smaller than the constellations of Hellenistic t ... References {{Reflist External links 香港太空館https://web.archive.org/web/20120813070951/http://www.lcsd.gov.hk/CE/Museum/Space/Research/c_index.htm 研究資源] *中國星區、星官及星名英譯表 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Vulpecula (constellation)
Vulpecula is a faint constellation in the northern sky. Its name is Latin for "little fox", although it is commonly known simply as the fox. It was identified in the seventeenth century, and is located in the middle of the Summer Triangle (an asterism (astronomy), asterism consisting of the bright stars Deneb, Vega, and Altair). Features Stars There are no stars brighter than 4th magnitude in this constellation. The brightest star in Vulpecula is Alpha Vulpeculae, a apparent magnitude, magnitude 4.44m red giant at a distance of 297 light-years. The star is an double star, optical binary (separation of 413.7") that can be split using binoculars. The star also carries the traditional name Anser, which refers to the goose the little fox holds in its jaws. 23 Vulpeculae is the second brightest star in the constellation. In 1967, the first pulsar, PSR B1919+21, was discovered in Vulpecula by Jocelyn Bell, supervised by Antony Hewish, in Cambridge, England, Cambridge. While they we ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
4 Vulpeculae
4 Vulpeculae is a single, orange-hued star in the northern constellation of Vulpecula. It forms part of the asterism, formerly thought to be an open cluster, called the coathanger or Brocchi's Cluster. The star is faintly visible to the naked eye with an apparent visual magnitude of 5.16. The distance to this star, based upon an annual parallax shift of , is around 260 light years. At the age of about 2.6 billion years old, this is an aging giant star with a stellar classification of K0 III, having exhausted the supply of hydrogen at its core and evolved off the main sequence. It is now a red clump giant, indicating that it is on the horizontal branch and is generating energy through the fusion of helium at its core. The star has an estimated 1.72 times the mass of the Sun and has expanded to 11.42 times the Sun's radius. It is radiating 67.6 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
13 Vulpeculae
13 Vulpeculae is a blue giant with a stellar classification of class B9.5III in the northern constellation Vulpecula. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 4.57 and it is approximately 339 light years away from the Sun based on parallax. The star is radiating 180 times the luminosity of the Sun from its photosphere at an effective temperature of 8,801 K. There is one reported companion, designated component B, with a magnitude of 7.37, an orbital period of roughly 615 years, and an angular separation of . The system is moving closer to the Earth with a heliocentric radial velocity The radial velocity or line-of-sight velocity, also known as radial speed or range rate, of a target with respect to an observer is the temporal rate of change, rate of change of the distance or Slant range, range between the two points. It is e ... of −28 km/s. References External links * {{DEFAULTSORT:1 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
16 Vulpeculae
16 Vulpeculae is a binary star system in the northern constellation Vulpecula. It has a combined apparent visual magnitude of 5.787, which is near the lower limit of visibility to the naked eye. Based upon an annual parallax shift of as seen from Earth's orbit, it is located about 222 light years away. The system is moving closer to the Sun with a heliocentric radial velocity of about −37 km/s. It will make its closest approach in about 0.9 million years, coming within . The pair orbit each other with an estimated period of 1,201 years and an orbital eccentricity of 0.932. The magnitude 5.93 primary, component A, displays a stellar classification of F2III, matching an aging F-type giant star. This star is spinning rapidly with a projected rotational velocity of 136 km/s. This is giving the star an oblate shape with an equatorial bulge that is an estimated 21% larger than the polar radius. It is 742 million years old with 1.34 times the mass o ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
20 Vulpeculae
20 Vulpeculae is single star located around 1,170 light years away in the northern constellation of Vulpecula. It is visible to the naked eye as a dim, blue-white hued star with an apparent visual magnitude of 5.91. The object is moving closer to the Earth with a heliocentric radial velocity of −22 km/s. This is a Be star with a stellar classification of B7 Ve. It is spinning rapidly with a projected rotational velocity of 236 km/s (compared to a critical velocity of 332 km/s) and has an estimated polar inclination of 71.1°. The star has four times the mass of the Sun and is radiating around 460 times the Sun's luminosity from its photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagnetic radiation. Effective temperature is often used as an estimate of a body's surface temperature ... of 12,050 K. Ref ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
19 Vulpeculae
19 Vulpeculae is star located approximately 1,690 light years from Earth in the northern constellation of Vulpecula. It is a probable member of the open cluster NGC 6882. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.40. It is moving closer to the Earth with a heliocentric radial velocity of −19 km/s. This is an aging giant star with a stellar classification of K2 IIIa, having already consumed the hydrogen at its core and evolved away from the main sequence. It has nearly five times the mass of the Sun but has expanded to around 100 times the Sun's radius. The star is radiating 2,889 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagnetic radiation. Effective temperature is often used as an estimate of a body' ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
18 Vulpeculae
18 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located about 489 light years away from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.51. The system is moving closer to the Earth with a heliocentric radial velocity of −11.7 km/s. This is a double-lined spectroscopic binary system with an orbital period of 9.3 days and a small eccentricity of 0.0116. It is a detached binary with a semimajor axis of . The system contains a Delta Scuti variable, but the temperature places it to the blue (hotter) side of the δ Scuti instability strip. The combined stellar classification of this system remains unclear, with classes of A3 III, A1 IV, A3 V, and A2 IV being given. The ultraviolet spectrum matches an A3 dwarf star A dwarf star is a star of relatively small size and low luminosity. Most main sequence stars are dwarf stars. The meaning of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
23 Vulpeculae
23 Vulpeculae is a triple star system in the northern constellation of Vulpecula. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.52 and it is located approximately 327 light years away from the Sun based on parallax. The system is moving further from the Earth with a heliocentric radial velocity of +1.47 km/s. Component A forms a binary system with an orbital period of 25.33 years, an eccentricity of 0.40, and a semimajor axis of . The 4.80 magnitude member of this pair, component Aa is an aging giant star with a stellar classification of , where the suffix indicates an underabundance of iron in the spectrum. This star has 2.4 times the mass of the Sun and is radiating 146 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagneti ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
21 Vulpeculae
21 Vulpeculae is a single, white-hued star in the northern constellation of Vulpecula. Its distance can be estimated from the annual parallax shift of , yielding a separation of 313 light years. The star is faintly visible to the naked eye at night, having an apparent visual magnitude of 5.19. It is moving further away with a heliocentric radial velocity of about +7 km/s, having come within around 4.2 million years ago. There is some disagreement about the class of this star. Cowley et al. (1969) listed it as an A-type subgiant star with a stellar classification of A7 IVn, where the 'n' notation indicates "nebulous" lines due to rapid rotation. The luminosity class of IV suggests the star has exhausted the supply of hydrogen at its core and is evolving away from the main sequence. Slettebak (1982) classified it as an A5 IV shell star and it was so regarded by Hauck & Jaschek (2000), while Abt & Morrell (1995) listed it with a class of A5 Vn ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
15 Vulpeculae
15 Vulpeculae is a variable star in the northern constellation of Vulpecula, located approximately 243 light years away based on parallax. It has the variable star designation NT Vulpeculae; ''15 Vulpeculae'' is the Flamsteed designation. It is visible to the naked eye as a faint, white-hued star with a typical apparent visual magnitude of 4.66. This object is moving closer to the Earth with a heliocentric radial velocity of −26 km/s. This is an Am star with a stellar classification of A4 IIIm, matching an evolved A-type giant star. However, Gray & Garrison (1989) found a class of kA5hA7mA7 (IV–V), which matches a blend of subgiant and main sequence luminosity classes with the K-line (kA5) of an A5 star and the hydrogen (hA7) and metal (mA7) absorption lines of an A7 star. It is an Alpha2 Canum Venaticorum-type variable with magnitude ranging from 4.62 down to 4.67 over a period of 14 days. The star is radiating 60 times the Sun's luminosity from its photo ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
CK Vulpeculae
CK Vulpeculae (also Nova Vulpeculae 1670) is an object whose exact nature is unknown. It was once considered to be the oldest reliably-documented nova. It consists of a compact central object surrounded by a bipolar nebula. Models suggest CK Vulpeculae may not be a classic nova; rather it may be classified as a luminous red nova which is the result of two main sequence stars colliding and merging. A 2018 study found it was most likely the result of an unusual collision of a white dwarf and a brown dwarf. A 2020 article ruled out this proposed mechanism and proposes that CK Vulpeculae is an intermediate luminosity optical transient, i.e. an object in the luminosity gap between supernovae and novae. Eruptive history CK Vulpeculae was discovered on June 20th 1670 by Voituret Anthelme and independently on July 25 by Johannes Hevelius. It had a brightness maximum of approximately magnitude 3 at its discovery after which it faded. A second maximum of approximately 2.6 mag ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
10 Vulpeculae
10 Vulpeculae is an astrometric binary star system in the northern constellation of Vulpecula. It is faintly visible to the naked eye with an apparent visual magnitude of 5.497. The system is located roughly 330 light years from the Sun, as determined from an annual parallax shift of . It is moving closer to the Sun with a heliocentric radial velocity of −9.9 km/s. The system is a source of X-ray emission. The visible component is an aging giant star with a stellar classification of G8 III. At the age of 1.15 billion years, it has exhausted the hydrogen at its core region and expanded off the main sequence. It is about 13 times the Sun's radius and 2.35 times the Sun's mass. The star is radiating 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature The effective temperature of a body such as a star or planet is the temperature of a black body that would emit the same total amount of electromagnetic radiation. Effe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
