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List Of Stars In Auriga ...
This is the list of notable stars in the constellation Auriga, sorted by decreasing brightness. See also *List of stars by constellation References * * * * * {{Stars of Auriga *List Auriga AURIGA (''Antenna Ultracriogenica Risonante per l'Indagine Gravitazionale Astronomica'') is an ultracryogenic resonant bar gravitational wave detector in Italy. It is at the Laboratori Nazionali di Legnaro of the Istituto Nazionale di Fisica Nuclea ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Star
A star is an astronomical object comprising a luminous spheroid of plasma held together by its gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye at night, but their immense distances from Earth make them appear as fixed points of light. The most prominent stars have been categorised into constellations and 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 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 total mass is the main factor determining its evolution and eventual fate. A star shines for most of its active life due t ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Multiple Star
A star system or stellar system is a small number of stars that orbit each other, bound by gravitational attraction. A large group of stars bound by gravitation is generally called a '' star cluster'' or ''galaxy'', although, broadly speaking, they are also star systems. Star systems are not to be confused with planetary systems, which include planets and similar bodies (such as comets). A star system of two stars is known as a ''binary star'', ''binary star system'' or ''physical double star''. If there are no tidal effects, no perturbation from other forces, and no transfer of mass from one star to the other, such a system is stable, and both stars will trace out an elliptical orbit around the barycenter of the system indefinitely. ''(See Two-body problem)''. Examples of binary systems are Sirius, Procyon and Cygnus X-1, the last of which probably consists of a star and a black hole. Multiple star systems A multiple star system consists of three or more stars that a ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Nu Aurigae
Nu Aurigae, Latinised from ν Aurigae, is the Bayer designation for a star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 3.96 and is approximately distant from the Earth. This is an evolved giant star with a stellar classification of G9.5 III. It is a red clump star, which indicates that it is generating energy through the fusion of helium at its core. The outer envelope has expanded to 19 times the radius of the Sun and cooled to , giving it the characteristic yellow-hued glow of a G-type star. It shines with 135 times the luminosity of the Sun. This is an astrometric binary with a suspected white dwarf companion. A 10th-magnitude star 54.6 arcseconds away is an optical companion. References External links HR 2012CCDM J05515+3909Image Nu Aurigae {{DEFAULTSORT:Nu Aurigae G-type giants Horizontal-branch stars Astrometric binaries Auriga (constellation) Aurigae, Nu Durchmusterung objects ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Aurigae
Delta Aurigae, Latinized from δ Aurigae, is the Bayer designation for an astrometric binary star in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 3.715. Based upon its annual parallax shift of , it is some distant from the Earth, give or take a three light-year margin of error. It is drifting further away with a radial velocity of +10 km/s. This star is the namesake for the Delta Aurigids, a meteor shower that occurs between October 6–15. The radiant point for this shower passes several degrees to the south of the star. The variable radial velocity of this system was not recognized until 1999, more than a century following the first measurement in 1897. Delta Aurigae is a single-lined spectroscopic binary: periodic Doppler shifts in the star's spectrum indicate orbital motion. The pair have an orbital period of and an eccentricity of 0.231. Based on the small amplitude of the radial velocity variati ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Aurigae
Zeta Aurigae, or ζ Aurigae, is a binary star system in the northern constellation of Auriga. Based upon parallax measurements made during the Hipparcos mission, this system is approximately distant from the sun. It has a combined apparent visual magnitude of 3.75, which is bright enough to be seen with the naked eye. The two components are designated Zeta Aurigae A (officially named Saclateni , an old misspelling of "Sadatoni") and B. Nomenclature ''ζ Aurigae'' ( Latinised to ''Zeta Aurigae'') is the system's Bayer designation. The designations of the two components as ''ζ Aurigae 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). The system bore the traditional names ''Haedus I'' (also ''Hoedus'') and ''Sadatoni'' (rarely ''Saclateni''). It was one of the two ''haedi'' (Latin: 'kids') of the she-goat Capella, the other being Haedus II, ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Aurigae
Eta Aurigae (η Aurigae, abbreviated Eta Aur, η Aur), officially named Haedus , is a star in the northern constellation of Auriga. With an apparent visual magnitude of 3.18, it is visible to the naked eye. Based upon parallax measurements made during the ''Hipparcos'' mission, this star is approximately distant from the Sun. Nomenclature ''η Aurigae'' ( Latinised to ''Eta Aurigae'') is the star's Bayer designation. Along with Zeta Aurigae it represents one of the kids of the she-goat Capella, from which it derived its Latin traditional name ''Haedus II'' or ''Hoedus II'', from the Latin ''haedus'' "kid" (Zeta Aurigae was Haedus I). It also had the less common traditional name ''Mahasim,'' from the Arabic المِعْصَم ''al-miʽşam'' "the wrist" (of the charioteer), which it shared with Theta Aurigae. In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the names ''Haedus'' f ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Aurigae
Epsilon Aurigae (ε Aurigae, abbreviated Epsilon Aur, ε Aur) is a multiple star system in the northern constellation of Auriga, the charioteer. It is an unusual eclipsing binary system comprising an F0 supergiant (officially named Almaaz , the traditional name for the system) and a companion which is generally accepted to be a huge dark disk orbiting an unknown object, possibly a binary system of two small B-type stars. The distance to the system is still a subject of debate, but data from the Gaia spacecraft puts its distance at around light years from Earth. Epsilon Aurigae was first suspected to be a variable star when German astronomer Johann Heinrich Fritsch observed it in 1821. Later observations by Eduard Heis and Friedrich Wilhelm Argelander reinforced Fritsch's initial suspicions and attracted attention to the star. Hans Ludendorff, however, was the first to study it in great detail. His work revealed that the system was an eclipsing binary variable, a s ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Iota Aurigae
Iota Aurigae (ι Aurigae, abbreviated Iota Aur, ι Aur), officially named Hassaleh , is a star in the northern constellation of Auriga. It has an apparent visual magnitude of 2.7, which is bright enough to be readily visible to the naked eye. Parallax measurements give a distance estimate of roughly from the Sun. Nomenclature ''ι Aurigae'' ( Latinised to ''Iota Aurigae'') is the star's Bayer designation. It bore the traditional name ''Al Kab'', short for ''Kabdhilinan'' , from the Arabic ʿAbd al-Raḥmān ibn ʿUmar al-Ṣūfīصور الكواكب الثابتة('' Book of Fixed Stars''). Manuscript from the National Library of France. "the ankleTranslation of the Arabic word كعب to English on the Almaany dictionaries website. of the [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpha² Canum Venaticorum Variable
An Alpha2 Canum Venaticorum variable (or α2 CVn variable) is a type of variable star. These stars are chemically peculiar main sequence stars of spectral class B8p to A7p. They have strong magnetic fields and strong silicon, strontium, or chromium spectral lines. Their brightness typically varies by 0.01 to 0.1 magnitudes over the course of 0.5 to 160 days. In addition to their intensities, the intensities and profiles of the spectral lines of α2 CVn variables also vary, as do their magnetic fields. The periods of these variations are all equal and are believed to equal the period of rotation of the star. It is thought that they are caused by an inhomogeneous distribution of metals in the atmospheres of these stars, so that the surface of the star varies in brightness from point to point. The type-star which this class is named after is α² Canum Venaticorum, a star in the binary system of Cor Caroli, which is in the northern constellation of Canes Venatici Canes Ven ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Theta Aurigae
Theta Aurigae ( Latinized from θ Aurigae, abbreviated Theta Aur, θ Aur) is a binary star in the constellation of Auriga. Based upon parallax measurements, the distance to this system is about . The two components are designated Theta Aurigae A (also named Mahasim) and B. Nomenclature ''θ Aurigae'' ( Latinised to ''Theta Aurigae'') is the system's Bayer designation. The designations of the two components as ''Theta Aurigae A'' and ''B'' derives from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU). Some authors state that Theta Aurigae had no traditional name,although Richard Hinckley Allen makes a passing reference about the name ''Mahasim'', as a name also used, with various spellings, for Eta Aurigae and Lambda Herculis, from the Arabic المِعْصَم ''al-miʽşam'' "the wrist" (of the charioteer). In 2016, the IAU organized a Working Group on Star Nam ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Algol Variable
Algol variables or Algol-type binaries are a class of eclipsing binary stars that are similar to the prototype member of this class, β Persei (Beta Persei, Algol). An Algol binary is a system where both stars are near-spherical such that the timing of the start and end of the eclipses is well-defined. The primary is generally a main sequence star well within its Roche lobe. The secondary may also be a main sequence star, referred to as a detached binary or it may an evolved star filling its Roche lobe, referred to as a semidetached binary. When the cooler component passes in front of the hotter one, part of the latter's light is blocked, and the total brightness of the binary, as viewed from Earth, temporarily decreases. This is the primary minimum of the binary. Total brightness may also decrease, but less so, when the hotter component passes in front of the cooler one; this is the secondary minimum. The period, or time span between two primary minima, is very regul ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eclipsing Binary
A binary star is a system of two stars that are gravitationally bound to and in orbit around each other. Binary stars in the night sky that are seen as a single object to the naked eye are often resolved using a telescope as separate stars, in which case they are called ''visual binaries''. Many visual binaries have long orbital periods of several centuries or millennia and therefore have orbits which are uncertain or poorly known. They may also be detected by indirect techniques, such as spectroscopy (''spectroscopic binaries'') or astrometry (''astrometric binaries''). If a binary star happens to orbit in a plane along our line of sight, its components will eclipse and transit each other; these pairs are called ''eclipsing binaries'', or, together with other binaries that change brightness as they orbit, ''photometric binaries''. If components in binary star systems are close enough they can gravitationally distort their mutual outer stellar atmospheres. In some cases, the ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
