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Equuleus (Chinese Astronomy)
According to traditional Chinese uranography, the modern constellation Equuleus is located within the northern quadrant of the sky, which is symbolized as the Black Tortoise of the North (北方玄武, ''Běi Fāng Xuán Wǔ''). The name of the western constellation in modern Chinese is 小馬座 (''xiǎo mǎ zuò''), meaning "the colt constellation". Stars The map of Chinese constellation in constellation Equuleus 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 linksEquuleus – Chinese associations https: ... [...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] |
Beta Equulei
Beta Equulei, Latinized from β Equulei, is the Bayer designation for a solitary star in the northern constellation of Equuleus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.16. The annual parallax shift is 11.27 mas, indicating a separation of around 289 light years from the Sun. It is drifting closer with a radial velocity of −11 km/s. This is an ordinary A-type main sequence star with a stellar classification of A3 V. It has 2.7 times the mass of the Sun and about four times the Sun's radius. The star is around 600 million years old – 93% of the way through its main sequence lifetime – and is spinning with a projected rotational velocity of 58 km/s. It is radiating 78 times the luminosity of the Sun from its photosphere at an effective temperature of about 9,000 K. The star emits an infrared excess indicating the presence of a dusty debris disk. The mean temperature of the dust is 85 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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 tradition. The Song dynasty (13th-century) Suzhou planisphere shows a total of 283 asterisms, comprising a total of 1,565 individual stars. The asterisms are divided into four groups, the Twenty-Eight Mansions (, ''Èrshíbā Xiù'') along the ecliptic, and the Three Enclosures of the northern sky. The southern sky was added as a fifth group in the late Ming Dynasty based on European star charts, comprising an additional 23 asterisms. The Three Enclosures (, ''Sān Yuán'') include the Purple Forbidden Enclosure, which is centered on the north celestial pole and includes those stars which could be seen year-round,Needham, J.Astronomy in Ancient and Medieval China. ''Philosophical Transactions of the Royal Society of London''. Series A, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Chinese Astronomy
Astronomy in China has a long history stretching from the Shang dynasty, being refined over a period of more than 3,000 years. The ancient Chinese people have identified stars from 1300 BCE, as Chinese star names later categorized in the twenty-eight mansions have been found on oracle bones unearthed at Anyang, dating back to the mid-Shang dynasty. The core of the "mansion" (宿 ''xiù'') system also took shape around this period, by the time of King Wu Ding (1250–1192 BCE). Detailed records of astronomical observations began during the Warring States period (fourth century BCE) and flourished from the Han period onward. Chinese astronomy was equatorial, centered on close observation of circumpolar stars, and was based on different principles from those in traditional Western astronomy, where heliacal risings and settings of zodiac constellations formed the basic ecliptic framework. Joseph Needham has described the ancient Chinese as the most persistent and accurate obser ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
6 Equulei
6 Equulei is a probable (95% chance) astrometric binary star system in the northern constellation of Equuleus, located 380 light years from the Sun. It is barely visible to the naked eye as a dim, white-hued star with an apparent visual magnitude of 6.07. The system is moving further away from the Earth with a heliocentric radial velocity of +6.9 km/s. It forms a wide optical double with γ Equulei, at an angular separation of 336 arcseconds in 2011. The visible component is an Ap star with a stellar classification of A2Vs, matching the evolutionary state of an A-type main sequence star while displaying "sharp" absorption lines. It is an estimated 970 million years old with a projected rotational velocity of 65 km/s. The star has 2.6 times the mass of the Sun and around 1.7 times the Sun's radius. It is radiating 71 times the luminosity of the Sun The solar luminosity (), is a unit of radiant flux ( power emitted in the form of photons) conv ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Equulei
Delta Equulei, Latinized from δ Equulei, is the second brightest star in the constellation Equuleus. Delta Equulei is a binary star system about 60 light years away, with components of class G0 and F5. Their combined magnitude is 4.47, and their absolute magnitude is 3.142. There is controversy as to the exact masses of the stars. One study puts the larger at 1.22 solar masses and the smaller at 1.17, while another pegs them at 1.66 and 1.593. The luminosity of the larger star is calculated to be 2.23 solar, and the smaller to be 2.17. System William Herschel listed Delta Equulei as a wide binary. Friedrich Georg Wilhelm von Struve later showed this to be an unrelated optical double star. However his son Otto Wilhelm von Struve Otto Wilhelm von Struve (May 7, 1819 (Julian calendar: April 25) – April 14, 1905) was a Russian astronomer of Baltic German origins. In Russian, his name is normally given as Otto Vasil'evich Struve (Отто Васильевич Струв ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Gamma Equulei
Gamma Equulei, Latinized from γ Equulei, is a double star in the northern constellation of Equuleus. It is located at a distance of around from Earth and is visible to the naked eye with a slightly variable apparent visual magnitude of around 4.7. The star is drifting closer to the Sun with a radial velocity of −16.5 km/s. Properties The primary component of γ Equulei is a chemically peculiar star with a stellar classification of . It has a spectrum corresponding to an A9 main sequence star, but with unusual abundances of strontium, chromium, and europium. Stars with this type of spectral peculiarity are called Ap stars. The abundances of some metals are believed to be due to chemical stratification in the slowly-rotating star, unusual for hot main sequence stars. A fairly wide range of spectral types have been published for γ Equulei, ranging from A5 to F1, some of them also indicating unusual abundances of iron in the spectrum. γ Equulei has particularly s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
9 Equulei
9 Equulei is an M-type star in the constellation Equuleus. It is an asymptotic giant branch (AGB) star, a star that has exhausted its core helium and is now fusing both hydrogen and helium in shells outside the core. It is also a suspected variable star with an amplitude of about 0.05 magnitudes. The spectral type is M2IIIa, meaning it is a relatively cool giant star. As an AGB star, it is burning hydrogen and helium in shells around an inert carbon-oxygen core. It has expanded to 58 times the radius of the Sun, and it radiates 720 times as much electromagnetic radiation from a photosphere with 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 . References {{DEFAULTSORT:9 Equulei Equuleus M-type giants Equulei, 09 105413 203291 8 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Equulei
Epsilon Equulei, Latinized from ε Equulei, is a star system of apparent magnitude +5.23 in the constellation of Equuleus. It is located 180 light years away from the Solar System, based on its parallax. Star system Two stars make up the brighter part of the Epsilon Equulei star system. They are called Epsilon Equulei A and B and are main-sequence stars of spectral type of F5 and F6, respectively. The orbital period of this binary is about 101.5 years. Although the average separation between the two stars is about , the orbit is remarkably eccentric, at 0.705. The two stars passed their periastron in 1920. Finally, it is thought that Epsilon Equulei A may be, in turn, a spectroscopic binary. The orbital period of the latter would be 2.03133 days. Approximately 10 arcseconds away from A and B is Epsilon Equulei C (HIP 103571), with an apparent magnitude of 7.35. It is another F-type main-sequence stars, and based on its similar distance and proper motion Proper moti ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Equuleus
Equuleus ( ) is a constellation of stars that are visible in the night sky. Its name is Latin for "little horse", a foal. Located just north of the celestial equator, it was one of the 48 constellations listed by the 2nd century astronomer Ptolemy, and remains one of the 88 modern constellations. It is the second smallest of the modern constellations (after Crux), spanning only 72 square degrees. It is also very faint, having no stars brighter than the fourth magnitude. Notable features Stars The brightest star in Equuleus is Alpha Equulei, traditionally called Kitalpha, a yellow star magnitude 3.9, 186 light-years from Earth. Its traditional name means "the section of the horse". There are few variable stars in Equuleus. Only around 25 are known, most of which are faint. Gamma Equulei is an alpha CVn star, ranging between magnitudes 4.58 and 4.77 over a period of around 12½ minutes. It is a white star 115 light-years from Earth, and has an optical companion of magnitude ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
3 Equulei
3 Equulei is a single star located in the small northern constellation of Equuleus. It is faintly visible to the naked eye at an apparent visual magnitude of 5.6. Based upon an annual parallax shift of 4.24 mas, 3 Equulei is roughly distant from Earth, give or take an 80 light-year margin of error. At that distance, the apparent brightness of the star is diminished by 0.15 in visual magnitude because of extinction from interstellar gas and dust. 3 Equulei has been referred to in some sources as ζ (Zeta) Equulei, although it was not given that designation by Bayer. Properties 3 Equulei is an evolved giant star with a stellar classification of K5 III. The measured angular diameter of this star, after correction for limb darkening, is . At the estimated distance of Delta Ophiuchi, this yields a physical size of about 63 times the radius of the Sun. It is radiating an estimated 949 times the luminosity of the Sun from this expanded outer envelope at an eff ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
4 Equulei
4 Equulei is a binary star system in the constellation of Equuleus, located about 3° to the east of Alpha Equulei. With an apparent visual magnitude of 5.94, it is just barely visible to the naked eye under good seeing conditions. The system shows an annual parallax shift of 20.44 mas as measured from Earth's orbit, which yields a distance estimate of about 160 light years. It is moving closer to the Sun with a radial velocity of −13 km/s. This is a single-lined spectroscopic binary with an orbital period of and an eccentricity of 0.39. The value of Where ''a'' is the actual semimajor axis and ''i'' is the orbital inclination. for the primary is , providing a lower bound for the semimajor axis. Griffin (2011) noted that the mass of the secondary component is likely to be at least equal to that of the Sun, which, for an ordinary main sequence star, should make it visible in the spectrum. The lack of significant ultraviolet emission appears to rule out a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
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