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Beta Lyrae variable

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Beta Lyrae variables are a class of close binary stars. [1]

31 relations: Algol variable, Amplitude, Apparent magnitude, Beta Lyrae, Binary star, Delta Pictoris, DV Aquarii, Eclipse, Giant star, Gravity, John Goodricke, Light curve, Light-year, List of variable stars, Mu1 Scorpii, Pi Scorpii, PU Puppis, Roche limit, Solar mass, Stellar classification, Stellar evolution, Stellar wind, Supergiant, Tau Canis Majoris, TU Muscae, Upsilon Sagittarii, UW Canis Majoris, V Puppis, Variable star, W Ursae Majoris variable, Zeta Andromedae.

Algol variables or Algol-type binaries are a class of eclipsing binary stars that are related to the prototype member of this class, β Persei (Beta Persei, Algol) from an evolutionary point of view.

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The amplitude of a periodic variable is a measure of its change over a single period (such as time or spatial period).

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The apparent magnitude (m) of a celestial object is a measure of its brightness as seen by an observer on Earth, adjusted to the value it would have in the absence of the atmosphere.

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Beta Lyrae (β Lyr, β Lyrae) is a binary star system approximately away in the constellation Lyra.

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A binary star is a star system consisting of two stars orbiting around their common center of mass.

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Delta Pictoris (δ Pic) is a blue giant star in the constellation Pictor.

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DV Aquarii is a Beta Lyrae type eclipsing binary.

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An eclipse is an astronomical event that occurs when an astronomical object is temporarily obscured, either by passing into the shadow of another body or by having another body pass between it and the viewer.

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A giant star is a star with substantially larger radius and luminosity than a main-sequence (or dwarf) star of the same surface temperature.

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Gravity or gravitation is a natural phenomenon by which all things with mass are brought towards (or 'gravitate' towards) one another including stars, planets, galaxies and even light and sub-atomic particles.

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John Goodricke FRS (17 September 1764 – 20 April 1786) was an English amateur astronomer.

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In astronomy, a light curve is a graph of light intensity of a celestial object or region, as a function of time.

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A light-year (abbreviation: ly), sometimes written light year, is a unit of length used informally to express astronomical distances.

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There are over 41,638 known variable stars (2008), with more being discovered regularly, so a complete list of every single variable is impossible at this place (cf. GCVS).

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Mu1 Scorpii (μ1 Sco, μ1 Scorpii) is a binary star system in the southern zodiac constellation of Scorpius.

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Pi Scorpii is a triple star system in the southern constellation Scorpius.

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PU Puppis (PU Pup) is a star in the constellation Puppis.

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The Roche limit (pronounced /ʁoʃ/ in IPA, similar to the sound of rosh), sometimes referred to as the Roche radius, is the distance within which a celestial body, held together only by its own gravity, will disintegrate due to a second celestial body's tidal forces exceeding the first body's gravitational self-attraction.

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The solar mass is a standard unit of mass in astronomy that is used to indicate the masses of other stars, as well as clusters, nebulae and galaxies.

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In astronomy, stellar classification is the classification of stars based on their spectral characteristics.

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Stellar evolution is the process by which a star changes during its lifetime.

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A stellar wind is a flow of gas ejected from the upper atmosphere of a star.

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Supergiants are among the most massive and most luminous stars.

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Tau Canis Majoris (τ CMa, τ Canis Majoris) is an eclipsing spectroscopic binary in the constellation Canis Major and the brightest star of an open cluster designated NGC 2362.

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TU Muscae, also known as HD100213, is a star in the constellation Musca.

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Upsilon Sagittarii (Upsilon Sgr, υ Sagittarii, υ Sgr) is a spectroscopic binary star system in the constellation Sagittarius.

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UW Canis Majoris is a star in the constellation Canis Major.

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V Puppis (V Pup) is a star system in the constellation Puppis.

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A variable star is a star whose brightness as seen from Earth (its apparent magnitude) fluctuates.

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A W Ursae Majoris variable, also known as a low mass contact binary, is a type of eclipsing binary variable star.

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Zeta Andromedae (Zeta And, ζ Andromedae, ζ And) is a star system in the constellation Andromeda.

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Redirects here:

Beta Lyrae Star, Beta Lyrae star, Beta Lyrae variables, Beta lyrae variable, W Serpentis star.

References

[1] https://en.wikipedia.org/wiki/Beta_Lyrae_variable

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