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List Of Stars In Cassiopeia
This is the list of notable stars in the constellation A constellation is an area on the celestial sphere in which a group of visible stars forms Asterism (astronomy), a perceived pattern or outline, typically representing an animal, mythological subject, or inanimate object. The origins of the e ... Cassiopeia, sorted by decreasing brightness. References * * * * * * * {{Stars of Cassiopeia *List Cassiopeia ... [...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] |
Beta Cassiopeiae
Beta Cassiopeiae (β Cassiopeiae, abbreviated Beta Cas or β Cas), officially named Caph , is a Delta Scuti variable star in the constellation of Cassiopeia. It is a giant star belonging to the spectral class F2. The white star of second magnitude (+2.28 mag, variable) has an absolute magnitude of +1.3 mag. Nomenclature ''Beta Cassiopeiae'' is the star's Bayer designation. It also bore the traditional names ''Caph'' (from the Arabic word ', "palm" - ''i.e.'' reaching from the Pleiades), ''Chaph'' and ''Kaff'', as well as ''al-Sanam al-Nakah'' "the Camel's Hump". 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 ''Caph'' for this star. Originally, the pre-Islamic Arabic term ''al-Kaff al-Khadib'' "the stained hand" referred to the five stars comprisin ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Alpha Cygni Variable
Alpha Cygni variables are variable stars which exhibit non-radial pulsations, meaning that some portions of the stellar surface are contracting at the same time other parts expand. They are supergiant stars of spectral types B or A. Variations in brightness on the order of 0.1 magnitudes are associated with the pulsations, which often seem irregular, due to beating of multiple pulsation periods. The pulsations typically have periods of several days to several weeks. The prototype of these stars, Deneb (α Cygni), exhibits fluctuations in brightness between magnitudes +1.21 and +1.29. Small amplitude rapid variations have been known in many early supergiant stars, but they were not formally grouped into a class until the 4th edition of the General Catalogue of Variable Stars was published in 1985. It used the acronym ACYG for Alpha Cygni variable stars. Many luminous blue variables (LBVs) show Alpha Cygni-type variability during their quiescent (hot) phases, but the LBV classi ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Kappa Cassiopeiae
Kappa Cassiopeiae (κ Cas, κ Cassiopeiae) is a star in the constellation Cassiopeia. κ Cassiopeiae has an unusual spectrum that has anomalously weak nitrogen lines, taken as an actual nitrogen deficiency in the atmosphere. This is indicated by the modified letter C on the assumption that it is also carbon-rich, although this might not actually be the case. It is also interpolated to BC0.7, being slightly hotter than a standard B1 star. κ Cassiopeiae is assumed to be a member of the Cassiopeia OB14 stellar association (Cas OB14) and treated as being at a distance of about , while its distance found from the Hipparcos parallax is about 1,400 parsecs. Its Gaia parallaxes are somewhat uncertain due to the brightness of the star, but a modern determination of the distance to Cas OB14 is . It is classified as an Alpha Cygni type variable star and its brightness varies by a few hundredths of a magnitude. Periods of two hours, 2.65 days, and nine days have been report ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
50 Cassiopeiae
50 Cassiopeiae is a white star in the northern constellation of Cassiopeia. In the past, it had been misidentified as a suspected nebula, and given the number NGC 771. The star is visible to the naked eye, having an apparent visual magnitude of +3.95. Based upon an annual parallax shift of , it is located 157 light years away. It is moving closer, having a heliocentric radial velocity of −18 km/s, and will approach to within in 1.879 million years. It is an A-type main-sequence star with a stellar classification of A2 V. It is a suspected variable star with a very small amplitude. 50 Cas has an estimated 2.56 times the mass of the Sun, and about 2.5 times the Sun's radius. It is radiating 64 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 tempe ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Zeta Cassiopeiae
Zeta Cassiopeiae, Latinized from ζ Cassiopeiae, and officially named Fulu , is a variable star in the constellation of Cassiopeia. It has a blue-white hue and is classified as a B-type subgiant with an apparent magnitude of +3.66. Based upon parallax measurements, it is approximately 590 light-years from the Sun. Nomenclature ''ζ Cassiopeiae'' ( Latinised to ''Zeta Cassiopeiae'') is the star's Bayer designation. In Chinese astronomy, Zeta Cassiopeiae is called 附路, Pinyin: Fùlù, meaning '' Auxiliary Road'', because this star is marking itself and standing alone in the ''Auxiliary Road'' asterism, '' Legs'' (mansion) (see : Chinese constellation). 附路 (Fùlù) was westernized into ''Foo Loo'', but that name was also designated for Eta Cassiopeiae by R.H. Allen, with the meaning of "a by-path" In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN approved the name ''Fulu'' for Zeta C ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
RS Canum Venaticorum Variable
An RS Canum Venaticorum variable is a type of variable star. The variable type consists of close binary stars having active chromospheres which can cause large stellar spots. These spots are believed to cause variations in their observed luminosity. Systems can exhibit variations on timescales of years due to variation in the spot surface coverage fraction, as well as periodic variations which are, in general, close to the orbital period of the binary system. Some systems exhibit variations in luminosity due to their being eclipsing binaries. Typical brightness fluctuation is around 0.2 magnitudes. They take their name from the star RS Canum Venaticorum (abbreviated RS CVn). Otto Struve (1946) first called attention to the group, but it was Oliver (1974) who was the first to formally propose a set of observational characteristics to define the RS CVn criteria. The working definition, as it is used today, was that set down by Hall (1976). Berdyuginabr>2.4 RS CVn stars/ref> The RS ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Eta Cassiopeiae
Eta Cassiopeiae (η Cassiopeiae, abbreviated Eta Cas, η Cas) is a binary star system in the northern constellation of Cassiopeia. Its binary nature was first discovered by William Herschel in August 1779. Based upon parallax measurements, the distance to this system is from the Sun. The two components are designated Eta Cassiopeiae A (officially named Achird , the traditional name for the system) and B. Nomenclature ''η Cassiopeiae'' ( Latinised to ''Eta Cassiopeiae'') is the system's Bayer designation. The designations of the two constituents as ''Eta Cassiopeiae A'' and ''B'' derive from the convention used by the Washington Multiplicity Catalog (WMC) for star systems, and adopted by the International Astronomical Union (IAU). The proper name ''Achird'' was apparently first applied to Eta Cassiopeiae in the Skalnate Pleso Atlas of the Heavens published in 1950, but is not known prior to that. Richard Hinckley Allen gives no historical names for the star ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Variable Star
A variable star is a star whose brightness as seen from Earth (its apparent magnitude) changes with time. This variation may be caused by a change in emitted light or by something partly blocking the light, so variable stars are classified as either: * Intrinsic variables, whose luminosity actually changes; for example, because the star periodically swells and shrinks. * Extrinsic variables, whose apparent changes in brightness are due to changes in the amount of their light that can reach Earth; for example, because the star has an orbiting companion that sometimes eclipses it. Many, possibly most, stars have at least some variation in luminosity: the energy output of the Sun, for example, varies by about 0.1% over an 11-year solar cycle. Discovery An ancient Egyptian calendar of lucky and unlucky days composed some 3,200 years ago may be the oldest preserved historical document of the discovery of a variable star, the eclipsing binary Algol. Of the modern astronomers, th ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Epsilon Cassiopeiae
Epsilon Cassiopeiae or ε Cassiopeiae, officially named Segin (), is a single star in the northern constellation of Cassiopeia. With an apparent visual magnitude of 3.4, this is one of the brightest stars in the constellation. The distance to this star has been determined directly using parallax measurements, yielding a value of around from the Sun. It is drifting closer with a radial velocity of −8 km/s. Nomenclature ''ε Cassiopeiae'', Latinised to ''Epsilon Cassiopeiae'', is the star's Bayer catalog designation. The star bore the traditional name ''Segin'', which probably originates from an erroneous transcription of ''Seginus'', the traditional name for Gamma Boötis, which itself is of uncertain origin. Different sources report varying pronunciations, with SEG-in the most common but the variants SAY-gin and seg-EEN also appearing. In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. The WGSN ... [...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 regular ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
Delta Cassiopeiae
Delta Cassiopeiae (δ Cassiopeiae, abbreviated Delta Cas, δ Cas) is an eclipsing binary star system in the northern circumpolar constellation of Cassiopeia. Based on parallax measurements taken during the Hipparcos mission, it is approximately from the Earth. Delta Cassiopeiae is the primary or 'A' component of a multiple star system designated WDS J01258+6014. Delta Cassiopeiae's two components are therefore designated WDS J01258+6014 Aa and Ab. Aa is officially named Ruchbah , the traditional name for the system. Nomenclature ''δ Cassiopeiae'' ( Latinised to ''Delta Cassiopeiae'') is the star's Bayer designation. WDS J01258+6014A is its designation in the Washington Double Star Catalog. It also bore the traditional names ''Ruchbah'' and ''Ksora''; the former deriving from the Arabic word ركبة ''rukbah'' meaning "knee", and the latter appeared in a 1951 publication, ''Atlas Coeli'' (Skalnate Pleso Atlas of the Heavens) by Czech astronomer Antonín Bečvář. Pro ... [...More Info...] [...Related Items...] OR: [Wikipedia] [Google] [Baidu] |
