Algol variable

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Algol variables or Algol-type binaries are a class of eclipsing binary stars where the orbital plane of the stars are coincident with the line of sight from Earth.[1] When the cooler component passes in front of the hotter one, part of the latter's light is blocked, and the total brightness of the binary, as viewed from Earth, temporarily decreases. This is the primary minimum of the binary. Total brightness may also decrease, but less so, when the hotter component passes in front of the cooler one; this is the secondary minimum.

The period, or time span between two primary minima, is very regular, being determined by the revolution period of the binary, the time it takes for the two components to once orbit around each other. Most Algol variables are quite close binaries, and therefore their periods are short, typically a few days. The shortest known period is 0.1167 days (~2:48 hours, HW Virginis); the longest is 9892 days (27 years, Epsilon Aurigae).

Component stars of Algol binary systems have a spherical, or slightly ellipsoidal shape. This distinguishes them from the so-called beta Lyrae variables and W Ursae Majoris variables, where the two components are so close that gravitational effects lead to serious deformations of both stars.

Generally the amplitudes of the brightness variations are of the order of one magnitude, the largest variation known being 3.4 magnitudes (V342 Aquilae). The components may have any spectrum, though in most cases the brighter component is found to have B, A, F, or G spectra.

Algol itself, the prototype of this type of variable star, Bayer designation Beta Persei, first had its variability recorded in 1667 by Geminiano Montanari. The mechanism for its being variable was first correctly explained by John Goodricke in 1782.

Many thousands of Algol binaries are now known: the latest edition of the General Catalogue of Variable Stars (2003) lists 3,554 of them (9% of all variable stars).

Designation (name) Constellation Discovery Apparent magnitude (Maximum)[2] Apparent magnitude (Minimum)[3] Range of magnitude Period Subtype Spectral types
(eclipsing components)
Comment
ε Aur Auriga J.H. Fritsch, 1821 2m.92 3m.83 0.91 27.08 years GS F0 Iab + ~ B5V  
U Cep Cepheus   6m.75 9m.24 2.49 2.49305 d  
R CMa Canis Major   5m.70 6m.34 0.64 1.13594 d SD triple system
S Cnc Cancer Hind, 1848 8m.29 10m.25 1.96 9.48455 d DS  
α CrB (Alphecca or Gemma) Corona Borealis   2m.21 (B) 2m.32 (B) 0.11 17.35991 d DM A0V + G5V  
U CrB Corona Borealis   7m.66 8m.79 1.13 3.45220 d SD  
u Her (68 Her) Hercules   4m.69 5m.37 0.68 2.05103 d SD  
VW Hya Hydra   10m.5 14m.1 3.6 2.69642 d SD  
δ Ori (Mintaka) Orion John Herschel, 1834 2m.14 2m.26 0.12 5.73248 d DM O9.5 II + B0.5III  
VV Ori Orion   5m.31 5m.66 0.35 1.48538 d KE  
β Per (Algol) Perseus Geminiano Montanari, 1669 2m.12 3m.39 1.27 2.86730 d SD B8V + K0IIV prototype, triple system
ζ Phe Phoenix   3m.91 4m.42 0.51 1.66977 d DM B6 V + B9 V probable quadruple system
U Sge Sagitta   6m.45 9m.28 2.83 3.38062 d SD  
λ Tau Taurus Baxendell, 1848 3m.37 3m.91 0.54 3.95295 d DM B3 V + A4 IV triple system
BL Tel Telescopium Luyten, 1935 7m.09 8m.08 0.99 778 d GS F4Ib+M one component may be variable
  • DM = A detached main-sequence system. Both components are main-sequence stars and neither fills their inner Roche lobe
  • DS = A detached system with a subgiant. The subgiant does not fill its inner critical surface
  • GS = A system with one or both giant and supergiant components; one of the components may be a main sequence star
  • KE = A contact system of early (O-A) spectral type, both components being close in size to their inner critical surfaces.

References[edit]

  1. ^ "A consideration of close binary systems in relation to light variation.". Report of the South African Association for the Advancement of Science 1: 110–111. 1903. Retrieved 11 August 2010. 
  2. ^ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))
  3. ^ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))