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Puppis (Chinese Astronomy)
According to traditional Chinese uranography, the modern constellation Puppis is located within the southern quadrant of the sky, which is symbolized as the Vermilion Bird of the South (南方朱雀, ''Nán Fāng Zhū Què''). The name of the western constellation in modern Chinese is 船尾座 (''chuán wěi zuò''), meaning "behind of the ship constellation". Stars The map of Chinese constellation in constellation Puppis area consists of: See also *Chinese astronomy * 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 linksPuppis – Chinese associations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 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Traditional Chinese Star Names
Chinese star names ( Chinese: , ''xīng míng'') are named according to ancient Chinese astronomy and astrology. The sky is divided into star mansions (, ''xīng xiù'', also translated as "lodges") and asterisms (, ''xīng guān''). The system of 283 asterisms under Three Enclosures and Twenty-eight Mansions was established by Chen Zhuo of the Three Kingdoms period, who synthesized ancient constellations and the asterisms created by early astronomers Shi Shen, Gan De and Wuxian. Since the Han and Jin Dynasties, stars have been given reference numbers within their asterisms in a system similar to the Bayer or Flamsteed designations, so that individual stars can be identified. For example, Deneb (α Cyg) is referred to as (''Tiān Jīn Sì'', the Fourth Star of Celestial Ford). In the Qing Dynasty, Chinese knowledge of the sky was improved by the arrival of European star charts. ''Yixiang Kaocheng'', compiled in mid-18th century by then deputy Minister of Rites Ignaz Kög ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
14 Puppis ...
This is the list of notable stars in the constellation Puppis, sorted by decreasing brightness. This constellation's Bayer designations (Greek-letter star names) were given while it was still considered part of the constellation of Argo Navis. After Argo Navis was broken up into Carina, Vela, and Puppis, these Greek-letter designations were kept, so that Puppis does not have a full complement of Greek-letter designations. For example, since Argo Navis's alpha star went to Carina, there is no Alpha Puppis. See also *List of stars by constellation References * * * * * * * {{DEFAULTSORT:List Of Stars In Puppis *List Puppis Puppis is a constellation in the southern sky. Puppis, the Latin translation of "poop deck", was originally part of an over-large constellation Argo Navis (the ship of Jason and the Argonauts), which centuries after its initial description, was ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Sigma Puppis
Sigma Puppis, Latinized from σ Puppis, is a binary star system in the southern constellation of Puppis. It has an apparent visual magnitude of 3.25, which is bright enough to be visible to the naked eye at night from the Southern Hemisphere. Through a telescope, it appears as a bright, orange-hued star with a nearby white companion. Parallax measurements indicate this star is located at a distance of about from Earth. This is a spectroscopic binary system, consisting of an orbiting pair of stars that have not been individually resolved with a telescope. Their orbital period is 257.8 days and the eccentricity is 0.17. The pair form an eclipsing binary of the Beta Lyrae type and a period of 130.5 days, or one half of their orbital period. The eclipse of the primary component causes a decline of 0.04 of a magnitude, while the secondary eclipse reduces the magnitude by 0.03. The combined stellar classification is K5 III, which matches the spectrum of a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 64440
HD 64440, also known as a Puppis, is a spectroscopic binary star in the constellation Puppis. Its apparent magnitude is 3.71. Located around distant, the primary is a bright giant A giant star is a star with substantially larger radius and luminosity than a main-sequence (or ''dwarf'') star of the same surface temperature.Giant star, entry in ''Astronomy Encyclopedia'', ed. Patrick Moore, New York: Oxford University Press ... of spectral type K1.5II and the secondary is an early A-type star. They orbit with a period just under 7 years and eccentricity 0.38. References Puppis K-type bright giants Spectroscopic binaries Puppis, a CD-40 3579 038414 3080 064440 A-type stars {{multi-star-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Puppis
Zeta Puppis (ζ Puppis, abbreviated Zeta Pup, ζ Pup), formally named Naos , is a star in the constellation of Puppis. The spectral class of O4 means this is one of the hottest, and most luminous, stars visible to the naked eye. It is one of the sky's few naked-eye class O-type stars as well as one of the closest to Earth. It is a blue supergiant, one of the most luminous stars in the Milky Way. Visually it is over 10,000 times brighter than the Sun, but its high temperature means that most of its radiation is in the ultraviolet and its bolometric luminosity is over 500,000 times that of the Sun. It is also the 72nd brightest star in terms of apparent magnitude from Earth. It is a runaway star, meaning it has an unusually large pace velocity, probably caused by being ejected from a close binary system when its companion exploded as a supernova. Naos is typical of O-type stars in having an extremely strong stellar wind, measured at 2,500 k ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
QZ Puppis
QZ Puppis (QZ Pup, b Pup) is a class B2.5V (blue main-sequence) star in the constellation Puppis (constellation), Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax. QZ Puppis was identified as a small-amplitude variable star in 1974, but the nature of the variability was unclear. It was thought to be a spectroscopic binary on the basis of variability in the radial velocity of its spectral lines. As a hot B-class main sequence star with variable spectral lines, it was suspected of being a β Cephei variable but this classification was repeatedly rejected. The short-period sinusoidal variations in brightness with an amplitude of 0.03 magnitudes were interpreted as Rotating ellipsoidal variable, ellipsoidal variations as the star, distorted by a close companion, rotates with a period of 1.1 days. Later analysis of Hipparcos photometry (astronomy), photometry detected shallow eclipses. The companion to QZ Puppis is only ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 61831
HD 61831 (d1 Puppis) is a class B2.5V (blue dwarf) star in the constellation Puppis Puppis is a constellation in the southern sky. Puppis, the Latin translation of "poop deck", was originally part of an over-large constellation Argo Navis (the ship of Jason and the Argonauts), which centuries after its initial description, was .... Its apparent magnitude is 4.84 and it is approximately 556 light years away based on parallax. References Puppis B-type main-sequence stars Puppis, d1 CD-38 3531 037297 2961 061831 {{Main-star-stub ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
3 Puppis
3 Puppis (3 Pup) is a supergiant star in the constellation Puppis. It is a very rare A supergiant, referred to as a B star despite its spectral classification, and its apparent magnitude is 3.93. 3 Puppis is surrounded by a disc of circumstellar dust, which is unusual for an A-type star. It is thought to be caused by a low mass companion. The companion is calculated to be a B8III - B6V star with a mass of , and its orbit has a semi major axis of 2.3 AU. Like most B stars, 3 Pup rotates rapidly, at 30% - 60% of the speed at which it would start to break apart. The disc has its inner edge only 3.8 AU from the primary star and it is suspected that deceleration of the hot primary stellar wind A stellar wind is a flow of gas ejected from the upper atmosphere of a star. It is distinguished from the bipolar outflows characteristic of young stars by being less collimated, although stellar winds are not generally spherically symmetric. D ... by the companion allows the du ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
