Search results
Results from the WOW.Com Content Network
Algol / ˈ æ l ɡ ɒ l /, [12] designated Beta Persei (β Persei, abbreviated Beta Per, β Per), known colloquially as the Demon Star, is a bright multiple star in the constellation of Perseus and one of the first non-nova variable stars to be discovered.
In stellar astronomy, the Algol paradox is a paradoxical situation when elements of a binary star seem to evolve in discord with the established theories of stellar evolution. [1] A fundamental feature of these theories is that the rate of evolution of stars depends on their mass: The greater the mass, the faster this evolution, and the more ...
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.
Looking Up: See the star Algol in the constellation Perseus slowly blink. Plus, enjoy a brilliant Jupiter and catch the Double Cluster full of stars.
Among the wonders easily visible on a January evening is the constellation Perseus, the Champion. At around 8 p.m., he is straight overhead as seen from mid-northern latitudes.
The Algol three-star system imaged in the near-infrared by the CHARA interferometer with 0.5 mas resolution in 2009. The shape of Algol C is an artifact. The shape of Algol C is an artifact. Algol A is being regularly eclipsed by the dimmer Algol B every 2.87 days.
The star system is the prototype of a group of eclipsing binary stars named Algol variables, though it has a third member to make up what is actually a triple star system. [18] The brightest component is a blue-white main-sequence star of spectral type B8V, [ 19 ] which is 3.5 times as massive and 180 times as luminous as the Sun . [ 18 ]
The second variable star to be described was the eclipsing variable Algol, by Geminiano Montanari in 1669; John Goodricke gave the correct explanation of its variability in 1784. Chi Cygni was identified in 1686 by G. Kirch , then R Hydrae in 1704 by G. D. Maraldi .