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An eclipsing binary star is a binary star system in which the orbital plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. [20] In the case where the binary is also a spectroscopic binary and the parallax of the system is known, the binary is quite valuable for stellar analysis.
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.
A binary system whose stars share an envelope may also be called an overcontact binary. [1] [2] The term "contact binary" was introduced by astronomer Gerard Kuiper in 1941. [3] Almost all known contact binary systems are eclipsing binaries; [4] eclipsing contact binaries are known as W Ursae Majoris variables, after their archetype star, W ...
Pages in category "Eclipsing binaries" ... Eclipsing binary; 0–9. 1 Persei; 2 Lyncis; 2MASS J05352184−0546085; 2M1510; Theta1 Orionis E; 7 Arietis; 9 Andromedae ...
The eclipsing binary pair is separated by only 0.062 astronomical units (au) from each other, whereas the third star in the system (Algol Ab) is at an average distance of 2.69 au from the pair, and the mutual orbital period of the trio is 681 Earth days. The total mass of the system is about 5.8 solar masses, and the mass ratios of Aa1, Aa2 ...
Mu 1 Scorpii is an eclipsing binary of the Beta Lyrae type. Discovered to be a spectroscopic binary by Solon Irving Bailey in 1896, it was only the third such eclipsing pair to be discovered. This is a semidetached binary system where the secondary is close to filling its Roche lobe, or it may even be overflowing.
In 2007, Patrick Wils et al. discovered that NSVS 14256825 is an eclipsing binary, by examining the Northern Sky Variability Survey (NSVS) data. They also classified it as an HW Virginis type star, a binary pair in which variability arises from one star reflecting the light of the other as they orbit each other. [6] [7] [8]
RR Caeli is an eclipsing binary star system, located 69 light-years from Earth in the constellation Caelum. It is made up of a red dwarf star and a white dwarf, which complete an orbit around each other every seven hours. There is evidence of two circumbinary planets orbiting even further away.