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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 / æ l ˈ m ɑː z /, the traditional name for the system) and a companion which is generally accepted to be a huge dark disk orbiting an unknown object ...
NSVS 14256825, also known as V1828 Aquilae, is an eclipsing binary system (of the Algol type) in the constellation of Aquila. The system comprises a subdwarf OB star and red dwarf star. The two stars orbit each other every 2.648976 hours. [1]
The following is a list of variable stars that are well-known, ... Eclipsing binary Algol type (EA/GS) R Aur: Auriga 6 m.7 13 m.9 7.2: 458 d Mira variable (M)
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.
TIC 168789840, also known as TYC 7037-89-1, [5] is a stellar system with six stars. [6] [4] Three pairs of binary stars circle a common barycenter.While other systems with three pairs of stars have been discovered, this was the first system where the stars can be observed eclipsing one another, as the Earth lies approximately on their planes of rotation.
The newly added stars (增 星, zēng xīng) were named as 增 一 (zēng yī, 1st added star), 增 二 (zēng èr, 2nd added star) etc. For example, γ Cephei is referred to as 少 衛 增 八 (Shào Wèi Zēng Bā, 8th Added Star of Second Imperial Guard). Some stars may have been assigned more than one name due to the inaccuracies of ...
Both stars (the filled regions) overfill their Roche lobes (enclosed by the black lines). A W Ursae Majoris variable, also known as a low mass contact binary, is a type of eclipsing binary variable star. These stars are close binaries of spectral types F, G, or K that share a common envelope of material and are thus in contact with one another.
Because AR Aurigae is an eclipsing binary (in fact, it is the only known eclipsing binary with a mercury-manganese star), accurate characterization of its parameters has been made possible. Based on the light-time effect observed from the stars, it is inferred that there is a third star with a mass of 0.54 M ☉ , orbiting at a separation of 13 ...