Search results
Results from the WOW.Com Content Network
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 ...
Phase-folded light curve of the Algol variable Zeta Phoenicis recorded by NASA's Transiting Exoplanet Survey Satellite (TESS) 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 ...
Light curves can be periodic, as in the case of eclipsing binaries, Cepheid variables, other periodic variables, and transiting extrasolar planets; or aperiodic, like the light curve of a nova, cataclysmic variable star, supernova, microlensing event, or binary as observed during occultation events. The study of the light curve, together with ...
The varying depths of J1407b's eclipses indicate its disk consists of various concentric rings and gaps of different opacities. A 2015 analysis of J1407b's eclipse light curve by Kenworthy and Mamajek found that J1407b's disk comprises at least 37 distinct rings with radii ranging from 0.2 to 0.6 AU (30 to 90 million km; 19 to 56 million mi).
In 2009, the AAVSO was awarded a three-year $800,000 grant from the NSF to run Citizen Sky, [10] a pro-am collaboration project examining the 2009-2011 eclipse of the star epsilon Aurigae. [11] The AAVSO headquarters was originally located at the residence of its founder William T. Olcott in Norwich, Connecticut.
The variable star is located in the constellation of Sagitta roughly 27,600 ly (8.5 kpc). [1] Current hypothesis and archival data suggest that Gaia17bpp belongs to a rare family of ultra-long period binary stars where the companion is enshrouded in large optically thick disks reminiscent of Epsilon Aurigae, VVV-WIT-07, and AS Leonis Minoris.
Examples of eclipsing binaries are Epsilon Aurigae (Almaaz), VV Cephei, and V766 Centauri (HR 5171). Angular diameter measurements can be inconsistent because the boundary of the very tenuous atmosphere differs depending on the wavelength of light in which the star is observed. [citation needed]
EO Aurigae is an eclipsing binary of Algol type in the northern constellation of Auriga. With a combined apparent magnitude of 7.71, [ 3 ] it is too faint to be seen with the unaided eye. The eclipsing binary nature of the star was detected in 1943 by Sergei Gaposchkin at Harvard College Observatory . [ 7 ]