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List Of Stars In Pegasus ...
This is the list of notable stars in the constellation Pegasus, sorted by decreasing brightness. See also * List of stars by constellation References * * * * * {{Stars of Pegasus *List Pegasus Pegasus ( grc-gre, Πήγασος, Pḗgasos; la, Pegasus, Pegasos) is one of the best known creatures in Greek mythology. He is a winged divine stallion usually depicted as pure white in color. He was sired by Poseidon, in his role as hor ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star
A star is an astronomical object comprising a luminous spheroid of plasma (physics), plasma held together by its gravity. The List of nearest stars and brown dwarfs, nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night sky, night, but their immense distances from Earth make them appear as fixed stars, fixed points of light. The most prominent stars have been categorised into constellations and asterism (astronomy), asterisms, and many of the brightest stars have proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. The observable universe contains an estimated to stars. Only about 4,000 of these stars are visible to the naked eye, all within the Milky Way galaxy. A star's life star formation, begins with the gravitational collapse of a gaseous nebula of material composed primarily of hydrogen, along with helium and trace amounts of heavier elements. Its stellar ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Pegasi
Epsilon Pegasi ( Latinised from ε Pegasi, abbreviated Epsilon Peg, ε Peg), formally named Enif , is the brightest star in the northern constellation of Pegasus. With an average apparent visual magnitude of 2.4, this is a second-magnitude star that is readily visible to the naked eye. The distance to this star can be estimated using parallax measurements from the Hipparcos astrometry satellite, yielding a value of around . Nomenclature ''ε Pegasi'' (Latinised to ''Epsilon Pegasi'') is the star's Bayer designation. It bore the traditional name ''Enif'' derived from the Arabic word for 'nose', due to its position as the muzzle of Pegasus. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016 included a table of the first two batches of names approved by the WGSN; which included ''Enif'' for this star. Other traditional names for the star i ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Xi Pegasi
Xi Pegasi (ξ Peg, ξ Pegasi) is the Bayer designation for a double star in the northern constellation of Pegasus, the winged horse. Located in the horse's neck, the primary component is an F-type main sequence star that is visible to the naked eye with an apparent visual magnitude of 4.2. It is 86% larger and 17% more massive that the Sun, radiating 4.5 times the solar luminosity. Based upon parallax measurements taken with the Hipparcos spacecraft, it is located 53.2 ± 0.2 light years from the Sun. The primary has been examined for the presence of an infrared excess that might indicate the presence of a debris disk, but none has been discovered. The common proper motion companion, NLTT 54820, is a twelfth magnitude red dwarf located at an angular separation Angular distance \theta (also known as angular separation, apparent distance, or apparent separation) is the angle between the two sightlines, or between two point objects as viewed from an observer. Angul ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kappa Pegasi
Kappa Pegasi (κ Peg, κ Pegasi) is a triple star system in the constellation Pegasus. It has an apparent brightness of +4.13 magnitude and belongs to the spectral class F5IV; a subgiant star. No proper name is associated to this star. This system consists of two components, designated Kappa Pegasi A and B, that are separated by an angular distance of 0.235 arcseconds. The binary nature of this pair was discovered by Sherburne W. Burnham in 1880. They orbit around each other every 11.6 years with a semimajor axis of 0.4 arcseconds. The brighter member of the pair, Kappa Pegasi B, is actually a spectroscopic binary, with the components designated Kappa Pegasi Ba and Kappa Pegasi Bb. They orbit about each other every six days. There is a fourth component, Kappa Pegasi C, which may be an optical companion In observational astronomy, a double star or visual double is a pair of stars that appear close to each other as viewed from Earth, especially with th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
1 Pegasi
1 Pegasi (1 Peg) is a triple star system in the constellation Pegasus, located approximately 156 light years away from the Sun based on parallax. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.09. The system is moving closer to the Earth with a heliocentric radial velocity of −11 km/s. The primary component is a giant with a stellar classification of K1III, a star that has exhausted the hydrogen supply at its core and evolved away from the main sequence. It has 1.57 times the mass of the Sun and has expanded to 12 times the Sun's radius. The star is radiating 72 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,600 K. There are several companions in addition to the primary. The brightest, component B, is a magnitude 9.3, K-type main-sequence star with a class of K0 V orbiting at an angular separation of 36.6" from the primary; it is itself a single-lined ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Lambda Pegasi
Lambda Pegasi (λ Peg, λ Pegasi) is a fourth-magnitude star in the constellation Pegasus. λ Pegasi is a yellow giant with stellar classification G8II-III. With a mass of and radius that is , the star boasts a bolometric luminosity that is roughly . Its apparent magnitude was calibrated in 1983 at 3.96, yielding an absolute magnitude of -1.45. Parallax calculations place the star at a distance of roughly 112 parsecs from Earth, or 365 ± 10 light years away, about three times the distance of its line-of-sight double μ Pegasi. In the constellation, Lambda and Mu lie to the southwest of Beta Pegasi Beta Pegasi (β Pegasi, abbreviated Beta Peg, β Peg), formally named Scheat , is a red giant star and the second-brightest star (after Epsilon Pegasi) in the constellation of Pegasus. It forms the upper right corner of the Great Square ..., the nearest bright star. References {{DEFAULTSORT:Lambda Pegasi Pegasi, Lambda G-type giants Pegasus (conste ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Iota Pegasi
ι Pegasi, Latinized as Iota Pegasi is a double-lined spectroscopic binary star system located within the northern constellation of Pegasus, along a line between Lambda and Kappa Pegasi. It is visible to the naked eye as a yellow-hued point of light with a combined apparent visual magnitude of 3.77. The system is located 38.5 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −5.5 km/s. The binary nature of this system was discovered by W. W. Campbell in 1899 and the initial orbital elements were estimated by H. D. Curtis in 1904. The primary, designated component Aa, is a yellowish-white star somewhat brighter than the sun. It and the dimmer component Ab orbit each other with a period of about 10 days and an eccentricity of almost zero, meaning they essentially have a circular orbit. They appear to be very young stars, close to zero-age main sequence. In about four billion years from now, component Aa will evol ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Theta Pegasi
θ Pegasi, Latinized as Theta Pegasi, is a single star in the equatorial constellation of Pegasus, lying about 7.5 degrees southwest of Enif. It has the traditional name Biham , and the Flamsteed designation 26 Pegasi. This object is visible to the naked eye as a white-hued point of light with an apparent visual magnitude of +3.52. The system is located 92 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −8 km/s. This object an A-type main-sequence star with a stellar classification of A2V. It is 448 million years old with a high rate of spin, showing a projected rotational velocity of 136 km/s. This star has 2.09 times the mass of the Sun and 2.6 times the Sun's radius. It is radiating 25 times the luminosity of the Sun from its outer envelope at an effective temperature of 7,951 K. The star appears to display a slight infrared excess. θ Pegasi was suspected of being a binary star due to an acc ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Mu Pegasi
Mu Pegasi or μ Pegasi, formally named Sadalbari (), is a star in the northern constellation of Pegasus. The apparent visual magnitude of this star is 3.5, which is bright enough to be seen with the naked eye even on a moonlit night. Based upon parallax measurements taken during the Hipparcos mission, it is approximately from the Sun. Nomenclature ''μ Pegasi'' ( Latinised to ''Mu Pegasi'') is the star's Bayer designation. It bore the traditional name ''Sadalbari'', which derives from ar, سعد بارع ''saʿd al-bāriʿ'', the “auspicious star of the splendid one.” In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name ''Sadalbari'' for this star on 21 August 2016 and it is now so included in the List of IAU-approved Star Names. In Chinese, (), meaning '' Resting Palace'', refers to an asterism consisting of Mu Pegasi, Lambda Pegasi, Omicron P ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Pegasi
Zeta Pegasi or ζ Pegasi, formally named Homam (), is a single star in the northern constellation of Pegasus. With an apparent visual magnitude of +3.4, this star is bright enough to be seen with the naked eye and is one of the brighter members of Pegasus. Parallax measurements place it at a distance of around from the Sun. Nomenclature ''ζ Pegasi'' ( Latinised to ''Zeta Pegasi'') is the star's Bayer designation. It bore the traditional name ''Homam'', meaning "Man of High Spirit" or "Lucky Star of High Minded". In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name ''Homam'' for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names. In Chinese, (), meaning '' Thunder and Lightning'', refers to an asterism consisting ζ Pegasi, ξ Pegasi, σ Pegasi, 55 Pegasi, 66 Pegasi and 70 Pegasi. Consequently, the Chinese ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Pegasi
Eta Pegasi or η Pegasi, formally named Matar , is a binary star in the constellation of Pegasus. The apparent visual magnitude of this star is +2.95, making it the fifth-brightest member of Pegasus. Based upon parallax measurements, the distance to this star is about from the Sun. Nomenclature ''η Pegasi'' ( Latinised to ''Eta Pegasi'') is the star's Bayer designation. It bore the traditional name ''Matar'', derived from the Arabic سعد المطر ''Al Saʽd al Maṭar'', meaning ''lucky star of rain''. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN) to catalogue and standardize proper names for stars. The WGSN approved the name ''Matar'' for this star on 21 August 2016 and it is now so entered in the IAU Catalog of Star Names. In Chinese, (), meaning '' Resting Palace'', refers to an asterism consisting η Pegasi, λ Pegasi, μ Pegasi, ο Pegasi, τ Pegasi and ν Pegasi. Consequently, η Pegasi itself is known as ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Beta Cephei Variable
Beta Cephei variables, also known as Beta Canis Majoris stars, are variable stars that exhibit small rapid variations in their brightness due to pulsations of the stars' surfaces, thought due to the unusual properties of iron at temperatures of 200,000 K in their interiors. These stars are usually hot blue-white stars of spectral class B and should not be confused with Cepheid variables, which are named after Delta Cephei and are luminous supergiant stars. Properties Beta Cephei variables are main-sequence stars of masses between about 7 and 20 M_\odot (that is, 7–20 times as massive as the Sun). Among their number are some of the brightest stars in the sky, such as Beta Crucis and Beta Centauri; Spica is also classified as a Beta Cephei variable but mysteriously stopped pulsating in 1970. Typically, they change in brightness by 0.01 to 0.3 magnitudes with periods of 0.1 to 0.3 days (2.4–7.2 hours). The prototype of these variable stars, Beta Cephei, shows variation in apparen ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
