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Perseus (Chinese Astronomy)
According to traditional Traditional Chinese star names#Categories of Chinese traditional uranography, Chinese uranography, the modern constellation Perseus (constellation), Perseus is located within the western quadrant of the sky, which is symbolized as the White Tiger (Chinese astronomy), White Tiger of the West (西方白虎, ''Xī Fāng Bái Hǔ''). The name of the western constellation in modern Chinese is 英仙座 (''yīng xiān zuò''), which means "the brave god constellation". Stars The map of Chinese constellation in constellation Perseus area consists of: See also *Chinese astronomy *Traditional Chinese star names *Chinese constellations References {{reflist External linksPerseus – 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/ 天文教育資訊網] *中國古天文* [...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] |
12 Persei
12 Persei (12 Per) is a double-lined spectroscopic binary star system in the northern constellation Perseus. Its combined apparent magnitude is 4.94, which means it can be viewed with the naked eye. Based upon parallax measurements, this system is about 79 light years away from the Sun. The magnitude difference between the two components is estimated to be 0.51. Based upon this, the primary has a mass around 138% of the Sun, 155% of the Sun's radius, and shines with three times the Sun's luminosity. The smaller secondary component is also larger than the Sun, with 124% of the Sun's mass, 131% of the radius of the Sun, and has 186% of the Sun's luminosity. The stellar classification of the primary is F9 V, which suggests it is an F-type main sequence star. The pair have an estimated age of just over a billion years. The pair orbit each other with a period of 331 days and an eccentricity of 0.663. The semimajor axis In geometry, the major axis of an e ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Persei
Eta Persei (η Persei, abbreviated Eta Per, η Per), is a binary star and the 'A' component of a triple star system (the 'B' component is the star HD 237009) in the constellation of Perseus. It is approximately 1331 light-years away from Earth. The two components of Eta Persei itself are designated Eta Persei A (officially named Miram , a recent name for the system) and B. Nomenclature ''η Persei'' ( Latinised to ''Eta Persei'') is the binary star's Bayer designation. The designations of its two components as ''Eta Persei A'' and ''B'' derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU). Eta Persei mysteriously gained the named ''Miram'' in the 20th Century, though no source is known. In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individua ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
30 Persei
30 Persei is a binary star system in the northern constellation Perseus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.49. Based upon an annual parallax shift of , is located roughly 730 light years from the Sun. It is a member of the Perseus OB3 association, which includes the Alpha Persei Cluster. This is a single-lined spectroscopic binary star system with an orbital period of 36.5 days and an eccentricity of roughly 0.3. The visible component is a B-type main-sequence star with a stellar classification of B7 V. It is spinning rapidly with a projected rotational velocity of 212 km/s. The star has 4.2 times the mass of the Sun and is radiating around 611 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 oft ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
32 Persei
32 Persei is a single star located 149 light years away from the Sun in the northern constellation of Perseus. It has the Bayer designation of l Persei, while ''32 Persei'' is the Flamsteed designation. This object is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 4.96. It is moving closer to the Earth with a heliocentric radial velocity of −9 km/s, and is a member of the Sirius supercluster: a stream of stars that share a common motion through space. This is an ordinary A-type main-sequence star with a stellar classification of A3V. It is around 125 million years old with a high rate of spin, showing a projected rotational velocity of 144 km/s. The star has double the mass of the Sun and 1.8 times the Sun's radius. It is radiating 21 times the luminosity of the Sun from its photosphere at an effective temperature of 8,872 K. References {{DEFAULTSORT:32 Persei A-type main-sequence stars Suspe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Omega Persei
Omega Persei (ω Persei) is a solitary, orange-hued star in the northern constellation of Perseus. The star is faintly visible to the naked eye with an apparent visual magnitude of +4.6. Based upon an annual parallax shift of 11.32 mas as seen from the Earth, the star is about 288 light years from the Sun. ω Persei has the traditional name Gorgonea Quarta , being the fourth member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus. This is an evolved K-type giant star with a stellar classification of K0 III. It is a red clump star that is generating energy via helium fusion at its core. At the estimated age of 1.65 billion years, Omega Persei has double times the mass of the Sun and has expanded to about 19 times the Sun's radius. It is radiating 144.5 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 tem ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
17 Persei
17 Persei is a single star in the northern constellation of Perseus, located about 390 light years away from the Sun. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.53. This object is moving further from the Earth at a heliocentric radial velocity of +13 km/s. Based upon a stellar classification of K5+III, this is an evolved giant star that has exhausted the hydrogen at its core. It is a suspected variable star, with an amplitude of 0.012 magnitude and period 4.4 days. The star has 1.3 times the mass of the Sun and has expanded to nearly 52 times the Sun's radius. It is radiating 551 times the luminosity of the Sun 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's surface te ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
20 Persei
20 Persei is a visual binary star in the northern constellation of Perseus, a few degrees from Pi Persei. It is visible to the naked eye as a dim, yellow-white hued point of light with a combined apparent visual magnitude of 5.343. The system is located around away from the Sun, based on its parallax. It is receding from the Earth with a heliocentric radial velocity of +6 km/s. The orbit of the two stars has been calculated from the secondary changing its position relative to the primary. The two orbit each other every 31.6 years with an angular semimajor axis In geometry, the major axis of an ellipse is its longest diameter: a line segment that runs through the center and both foci, with ends at the two most widely separated points of the perimeter. The semi-major axis (major semiaxis) is the longe ... of 0.22 arcseconds and an eccentricity of 0.7560. The combined spectrum of 20 Persei matches that of an F-type main-sequence star, and the two star ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Theta Persei
Theta Persei (Theta Per, θ Persei, θ Per) is a star system 37 light years away from Earth, in the constellation Perseus. It is one of the closest naked-eye stars. The primary star is a yellowish dwarf (main sequence) star of spectral type F8V, which is somewhat larger and brighter than the Sun, but still within the range considered to have the potential for Earth-like planets. There is also a red dwarf companion of spectral type M1.V, orbiting about 250 AU from the primary. It has a Gaia Data Release 2 parallax of , corresponding to a distance of . An 11th-magnitude star is listed in double-star catalogues as component C of the multiple system. It was away from component A in 2002, although the separation is rapidly increasing as it is a distant background object with a very different proper motion Proper motion is the astrometric measure of the observed changes in the apparent places of stars or other celestial objects in the sky, as seen ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
4 Persei
4 Persei is a single star in the northern constellation of Perseus, located around 670 light years away from the Sun. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of 5.04 The Bayer designation for this star is g Persei; ''4 Persei'' is the Flamsteed designation. This object has a peculiar velocity of 26.3 km/s and may be a runaway star. The stellar classification for 4 Persei is B8 III, matching an aging B-type giant star that has evolved off the main sequence. It is spinning with a projected rotational velocity of 60 km/s and has about 3.2 times the Sun's radius The star is radiating 670 times the luminosity of the Sun 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 su ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1 Persei
1 Persei (1 Per) is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear. Observational history The possible eclipsing binary nature of 1 Persei was first noticed by Donald Kurtz Donald Wayne Kurtz (1948 – ) is an astronomer known for his research into asteroseismology. He completed his PhD in astronomy at the University of Texas in 1976 before moving to Cape Town, where he became a professor at the University of Cape ... in 1977 when it was used as a comparison star to test for photometric variability of HD 11408. In 1979 French amateur observers succeeded in determining an orbital period of 25.9 days. During the primary eclipse, the brightness drops to magnitude 5.85 ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
