Algol variable


Algol variables or Algol-type binaries are a class of eclipsing binary stars that are related to the prototype member of this class, β Persei from an evolutionary point of view. An Algol binary is a semidetached binary system where the primary component is an early type, main sequence star that does not fill its Roche lobe, while the cooler, fainter, larger, less massive secondary component lies above the main sequence in a Hertzsprung–Russell diagram and fills the Roche lobe. Early in its history, the secondary star would have been more massive, evolving first to overfill its Roche lobe. After rapid mass exchange, the lobe-filling star became less massive than its companion.
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 over moderate periods of time, 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 ; the longest is 9892 days. 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.
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. 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 lists 3,554 of them.
Designation ConstellationDiscoveryApparent magnitude Apparent magnitude Range of magnitudePeriodSubtypeSpectral types
Comment
ε AurAurigaJ.H. Fritsch, 18212m.923m.8327.08 yearsGSF0 Iab + ~ B5V
U CepCepheus 6m.759m.24 d -
R CMaCanis Major 5m.706m.34 dSDtriple system
S CncCancerHind, 18488m.2910m.25 dDS
α CrB Corona Borealis 2m.21 2m.32 dDMA0V + G5V
U CrBCorona Borealis 7m.668m.79 dSD
u Her Hercules 4m.695m.37 dSD
VW HyaHydra 10m.514m.1 dSD
δ Ori OrionJohn Herschel, 18342m.142m.26 dDMO9.5 II + B0.5III
VV OriOrion 5m.315m.66 dKE
β Per PerseusGeminiano Montanari, 16692m.123m.39 dSDB8V + K0IIVprototype, triple system
ζ PhePhoenix 3m.914m.42 dDMB6 V + B9 Vprobable quadruple system
U SgeSagitta 6m.459m.28 dSD
λ TauTaurusBaxendell, 18483m.373m.91 dDMB3 V + A4 IVtriple system
δ VelVelaOtero, Fieseler, 20001m.962m.39 dDMA2 IV + A4 Vtriple, probable quintuple system
BL TelTelescopiumLuyten, 19357m.098m.08778 dGSF4Ib+Mone component may be variable