eclipsing binary star


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Related to eclipsing binary star: visual binary, Binary star system

eclipsing binary star:

see binary starbinary star
or binary system,
pair of stars that are held together by their mutual gravitational attraction and revolve about their common center of mass. In 1650 Riccioli made the first binary system discovery, that of the middle star in the Big Dipper's handle, Zeta
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; variable starvariable star,
star that varies, either periodically or irregularly, in the intensity of the light it emits. Other physical changes are usually correlated with the fluctuations in brightness, such as pulsations in size, ejection of matter, and changes in spectral type, color, or
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.
References in periodicals archive ?
This is how wobbling eclipsing binary stars are being weeded out.
Our volunteers have also discovered new RR Lyrae variable stars, dwarf novae, and eclipsing binary stars.
For eclipsing binary stars the recommended minimum interval can be as little as 30, 20 or even 10 minutes during eclipse, depending upon the rapidity of the fade and rise.
Prozesky, did a project on eclipsing binary stars under the supervision of Smits.
She had met Cline in 1999 when she was a graduate student in astrophysics at the University of North Carolina at Chapel Hill and was designing an experiment to study sets of variable and eclipsing binary stars. She had the equipment, the money, and the motivation, everything she needed to work on her thesis--except a dark spot to install her equipment.
There are several favourable minima of eclipsing binary stars during August and September, including Algol (P [Beta] Persei), [delta] [Delta] Tauri, and RZ Cassiopeiae.
Eclipsing binary stars are rich sources of information on the intrinsic properties of stars.
False alarms are often caused by starspots or other stellar surface activity, grazing eclipsing binary stars, or a separate eclipsing binary close to the target star.
Unlike in other eclipsing binary stars, Epsilon Aurigae's light is blocked not by a companion star but, apparently, by something gigantic, dark, and very elongated with a hole in the middle.
Swedish astronomer Edvard Hugo von Zeipel first predicted this "gravity darkening" in 1924, and Henry Norris Russell obtained the first observational evidence for it in 1939 from the light curves of eclipsing binary stars with rapidly rotating components.