Astronomy:Algol variable

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Short description: Class of eclipsing binary stars
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-spherical such that the timing of the start and end of the eclipses is well-defined. The primary is generally a main sequence star well within its Roche lobe. The secondary may also be a main sequence star, referred to as a detached binary or it may an evolved star filling its Roche lobe, referred to as a semidetached binary.[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.[2]

The period, or time span between two primary minima, is very regular over moderate periods of time (months to years), 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). Over long periods of time, various effects can cause the period to vary: in some Algol binaries, mass transfer between the closely spaced components of the variable may cause monotonic increases in period; if one component of the pair is magnetically active, the Applegate mechanism may cause recurrent changes in period on the order of ∆P/P ≈ 10−5; magnetic braking or the effects of a third component star in a highly eccentric orbit can cause larger changes in period.[3]

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 spectral type, though in most cases the brighter component is found to have a B, A, F, or G class.

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).

This is a dynamic list and may never be able to satisfy particular standards for completeness. You can help by expanding it with reliably sourced entries.
Designation (name) Constellation Discovery Apparent magnitude (Maximum)[nb 1] Apparent magnitude (Minimum)[nb 2] 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 + K0IV 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
δ Vel Vela Otero, Fieseler, 2000 1m.96 2m.39 0.43 45.15 d DM A2 IV + A4 V triple, probable quintuple system
TX Leonis Leo Meyer, Ernst-Joachim, 1933 5m.66 5m.75 0.09 2.445 d DM A2V triple system
BL Tel Telescopium Luyten, 1935 7m.09 8m.08 0.99 778 d GS F4Ib+M one component may be variable
  1. ↑ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))
  2. ↑ (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))
  • 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.
  • SD = A semidetached system. One star fills its Roche lobe.

References

  1. ↑ "GCVS Variability Types". General Catalogue of Variable Stars. http://www.sai.msu.su/gcvs/gcvs/vartype.htm. 
  2. ↑ Andronov, I. L. (2012). "Phenomenological modeling of the light curves of algol-type eclipsing binary stars". Astrophysics 55 (4): 536. doi:10.1007/s10511-012-9259-0. Bibcode: 2012Ap.....55..536A. 
  3. ↑ Applegate, James H. (1992). "A mechanism for orbital period modulation in close binaries". Astrophysical Journal, Part 1 385: 621–629. doi:10.1086/170967. Bibcode: 1992ApJ...385..621A. 

Further reading



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