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Camelopardalis (Chinese Astronomy)
According to traditional Chinese uranography, the modern constellation Camelopardalis is located in Three Enclosures (三垣, ''Sān Yuán'') The name of the western constellation in modern Chinese is 鹿豹座 (''lù bào zuò''), meaning "the leopard-deer constellation". Stars The map of Chinese constellation in constellation Camelopardalis 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 linksCamelopardalis – 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] *中國星區、星官及星名英譯表*台灣自然科學博物館http://aeea.nmns.edu.tw/ 天文� ... [...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] |
CO Camelopardalis
HD 106112, also known as CO Camelopardalis, is a star in the constellation Camelopardalis. It has an apparent magnitude of about 5.1, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is around 177 light years away from the Sun. HD 106112's spectral type shows that it is an A-type giant star. HD 106112 is also an Am star, also known as a metallic-line star. These types of stars have spectra indicating varying amounts of metals, like iron. Observations of the stars spectrum reveal a periodic Doppler shift. This means that HD 106112 is a spectroscopic binary with a period of 1.271 days and an eccentricity of 0.01. In fact, the two stars orbit so closely that they distort each other into an ellipsoidal shape through gravity, thereby forming a rotating ellipsoidal variable Rotating ellipsoidal variables are a class of variable star. They are close binary systems whose components a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 26670
HD 26670, also known as HR 1305, is a star located in the northern circumpolar constellation of Camelopardalis, the giraffe. The object has been designated as 26 H. Camelopardalis, but is not commonly used in modern times. It has an apparent magnitude of 5.70, allowing it to be faintly visible to the naked eye. Based on parallax measurements from Gaia DR3, the object is estimated to be 491 light years away from the Solar System. It appears to be slowly receding with a heliocentric radial velocity of . Characteristics This is a solitary, bluish-white hued B-type main-sequence star with a stellar classification of B7 V. It has also been given a class of B5 Vn with the addition of broad or nebulous absorption lines due to rapid rotation. It has 4 times the mass of the Sun and is estimated to be 57 million years old, having completed only a quarter of its main sequence lifetime. HD 26670 has 2.86 times the radius of the Sun and an effective temperature of . When combined ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
HD 24480
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HD 24480 is a multiple star system in the northern constellation of Camelopardalis. The brighter component is a giant star with a stellar classification of K4III and an apparent magnitude of 5.20. The companion is a hotter, A- or B-type star that is a suspected spectroscopic binary system. The visible pair have an angular separation of . References External links HR 1205CCDM J03571+6107Image HD 24480 K-type giants Double stars Camelopardalis Durchmusterung objects 024480 018488 1205 Year 1205 ( MCCV) was a common year starting on Saturday (link will display the full calendar) of the Julian calendar. Events By place Byzantine Empire * Spring – Theodore I (Laskaris) is proclaimed Byzantine emperor (or '' b ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
D Camelopardalis
HD 21447 is a probable binary star system located in the constellation Camelopardalis. The star is also known as HR 1046. It can be viewed with the naked eye, having an apparent visual magnitude of 5.09. Based upon an annual parallax shift of , it is located some 199 light years from the Sun. It is a candidate for membership in the Ursa Major Moving Group. The primary component is A-type main-sequence star with a stellar classification of A1 Va. It is around 146 million years old and is spinning with a projected rotational velocity of 182 km/s. The star has an estimated 2.32 times the mass of the Sun and about 1.9 times the Sun's radius. It is radiating around 32 times the Sun's luminosity from its photosphere at an effective temperature of 10,049 K. The companion is visual magnitude 9.4 star at an angular separation of . References External links *http://www.alcyone.de/cgi-bin/search.pl?object=HR1046 *http://server3.wikisky.org/starview? ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
CE Camelopardalis
HD 21389 is a supergiant variable star in reflection nebula VdB 15, in the constellation Camelopardalis. It has the variable star designation CE Camelopardalis, abbreviated CE Cam. This object is part of the Camelopardalis OB1 association. The near-identical member CS Camelopardalis lies half a degree to the north. Since 1943, the spectrum of CE Cam has served as one of the stable anchor points by which other stars are classified. CE Camelopardalis is some 19 times as massive as the Sun and 55,000 timers as luminous. Hohle and colleagues, using the parallax, extinction and analysis of spectrum, came up with a mass 14.95 ± 0.41 times that and luminosity 62,679 times that of the Sun. CE Cam is embedded in a large dusty molecular cloud, part of which it illuminates as a reflection nebula (vdB15 or BFS 29). This is a region of ongoing star formation with stars aged from one to a hundred million years old. CE Cam itself is thought to be around 11 million years ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
CS Camelopardalis
CS Camelopardalis (CS Cam; HD 21291) is a binary star in reflection nebula VdB 14, in the constellation Camelopardalis. It forms a group of stars known as the Camelopardalis R1 association, part of the Cam OB1 association. The near-identical supergiant CE Camelopardalis is located half a degree to the south. The primary component, CS Camelopardalis A, is a blue-white B-type supergiant with a mean apparent magnitude of 4.21m. It is classified as an Alpha Cygni type variable star and its brightness varies from magnitude 4.19m to 4.23m. Its companion, CS Camelopardalis B, is a magnitude 8.7m star located 2.4 arcseconds from the primary. References External links Image CS CamelopardalisNebula vdB 14 {{DEFAULTSORT:CS Camelopardalis 021291 016228 Alpha Cygni variables Binary stars B-type supergiants Camelopardalis Camelopardalis, CS 1035 Year 1035 ( MXXXV) was a common year starting on Wednesday (link will display the full calendar) of the Julia ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gamma Camelopardalis
Gamma Camelopardalis, Latinized from γ Camelopardalis, is a suspected wide binary star system in the northern circumpolar constellation of Camelopardalis. With a visual magnitude of 4.66, it is faintly visible to the naked eye. Based upon an annual parallax shift of 9.09 mas as seen from Earth, this star is located about 359 light years from the Sun. The brighter primary, designated component A, is a white-hued A-type subgiant star with a stellar classification of A2 IVn. It is spinning rapidly with a projected rotational velocity of 205 km/s. This is giving the star an oblate shape with an equatorial bulge that is 17% larger than the polar radius. It has about three times the mass of the Sun and 2.5 times the Sun's radius. The star is radiating 185 times the Sun's luminosity from its photosphere at an effective temperature of 8,892 K. The magnitude 9.07 secondary, BD+70 260, designated component C, lies at an angular separation of ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
BN Camelopardalis
BN Camelopardalis is a suspected astrometric binary in the northern circumpolar constellation of Camelopardalis. It appears as a variable star that is visible to the naked eye as a dim, white-hued point of light with an apparent visual magnitude that fluctuates around 5.49. The system is located at a distance of around 310 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +9 km/s. The visible component is a weakly magnetic chemically peculiar star with a stellar classification of B9.5VpSi, matching a B-type main-sequence star with an anomalous abundance of silicon. It is a variable star that ranges in brightness from 5.34 down to 5.58. Samus et al. (2017) have it categorized as an α2 Canum Venaticorum variable with a period of 2.7347 days, while Adelman and Sutton (2007) found a period of 2.73501 days. The star has three times the mass and radius of the Sun and is radiating 110 times the Sun's lum ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
K Camelopardalis
K, or k, is the eleventh letter in the Latin alphabet, used in the modern English alphabet, the alphabets of other western European languages and others worldwide. Its name in English is ''kay'' (pronounced ), plural ''kays''. The letter K usually represents the voiceless velar plosive. History The letter K comes from the Greek letter Κ (kappa), which was taken from the Semitic kaph, the symbol for an open hand. This, in turn, was likely adapted by Semitic tribes who had lived in Egypt from the hieroglyph for "hand" representing /ḏ/ in the Egyptian word for hand, ⟨ ḏ-r-t⟩ (likely pronounced in Old Egyptian). The Semites evidently assigned it the sound value instead, because their word for hand started with that sound. K was brought into the Latin alphabet with the name ''ka'' /kaː/ to differentiate it from C, named ''ce'' (pronounced /keː/) and Q, named ''qu'' and pronounced /kuː/. In the earliest Latin inscriptions, the letters C, K and Q were all ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
VZ Camelopardalis
VZ Camelopardalis is a single, variable star in the northern circumpolar constellation of Camelopardalis. It has a reddish hue and is faintly visible to the naked eye with an apparent visual magnitude that fluctuates around 4.92. The star is located at a distance of approximately 500 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s. It was considered a member of the Hyades Supercluster, but in 1990 this was brought into question. This object is an aging red giant star on the asymptotic giant branch with a stellar classification of M4IIIa. Its variable nature was discovered by American astronomer J. Ashbrook in 1948. This is a suspected slow irregular variable of sub-type Lb that varies in visual magnitude from 4.80 down to 4.96. Long-term photometry measurements suggest there are at least four pulsation periods ranging from 27.1 to 39.0 days. With the supply of hydrogen at its core exhausted the st ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
