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Studies of Algol led to the Algol paradox in the theory of stellar evolution: although components of a binary star form at the same time, and massive stars evolve much faster than the less massive stars, the more massive component Algol Aa1 is still in the main sequence, but the less massive Algol Aa2 is a subgiant star at a later evolutionary ...
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 ...
These 'Diagonal star tables' or star charts are also known as 'diagonal star clocks'. In the past they have also been known as 'star calendars', or 'decanal clocks'. [10] These star charts featuring the paintings of Egyptian deities, decans, constellations, and star observations are also found on the ceilings of tombs and temples.
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.
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 ...
The Indestructibles (Ancient Egyptian: j.ḫmw-sk – literally "the ones not knowing destruction" [1] [2]) was the name given by ancient Egyptian astronomers to two bright stars which, at that time, could always be seen circling the North Pole. [3]
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. By 1786, ten variable stars were known.