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 ...
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).
Book plate by Sidney Hall depicting Ursa Major's stars A light curve for Epsilon Ursae Majoris, plotted from TESS data [11] According to Hipparcos, Epsilon Ursae Majoris is 81 light-years (25 parsecs) from the Sun. Its spectral type is A1p; the "p" stands for peculiar, as its spectrum is characteristic of an α 2 Canum Venaticorum variable ...
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 ...
It has the Bayer designation α Aurigae, which is Latinised to Alpha Aurigae and abbreviated Alpha Aur or α Aur. Capella is the sixth-brightest star in the night sky, and the third-brightest in the northern celestial hemisphere after Arcturus and Vega. A prominent object in the northern winter sky, it is circumpolar to observers north of 44°N.
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]
LY Aurigae is a close visual binary. The two stars are magnitude 6.85 [7] and magnitude 8.35 [8] 0.6 arc-seconds apart. Each star is also a spectroscopic binary. A visual band light curve for LY Aurigae, adapted from Mayer et al. (2013) [9] In 1965, Pavel Mayer reported that the star, then called HD 35921, is a variable star.
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 ]