W Ursae Majoris variable

Schematic of a W Ursae Majoris variable with a mass ratio of 3. Both stars (the filled regions) overfill their Roche lobes (enclosed by the black lines).

A W Ursae Majoris variable, also known as a low mass contact binary, is a type of eclipsing binary variable star. These stars are close binaries of spectral types F, G, or K that share a common envelope of material and are thus in contact with one another. They are termed contact binaries because the two stars touch and transfer mass and energy through the connecting neck, although astronomer R.E. Wilson argues that the term "overcontact" is more appropriate.[1]

The class is divided into two subclasses: A-type and W-type[2] A-type W UMa binaries are composed of two stars both hotter than the Sun, having spectral types A or F, and periods of 0.4 to 0.8 day. The W-types have cooler spectral types of G or K and shorter periods of 0.22 to 0.4 day. The difference between the surface temperatures of the components is less than several hundred kelvins. A new subclass was introduced in 1978: B-type. The B-types have larger surface temperature difference. In 2004 the H (high mass ratio) systems were discovered by Sz. Csizmadia and P. Klagyivik.[3] The H-types have a higher mass ratio than ( = (secondary's mass)/(primary's mass)) and they have extra angular momentum.

These stars were first shown to follow a period-color relation (shorter period systems are redder) by Olin J. Eggen.[4] In 2012, Terrell, Gross and Cooney published a color-survey of 606 W UMa systems in the Johnson-Cousins photometric system.[5]

Their light curves differ from those of classical eclipsing binaries, undergoing a constant ellipsoidal variation rather than discrete eclipses. This is because the stars are gravitationally distorted by one another, and thus the projected area of the stars is constantly changing. The depths of the brightness minima are usually equal because both stars have nearly equal surface temperatures.

W Ursae Majoris is the prototype of this class.

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)[6] Apparent magnitude (Minimum)[6] Range of magnitude Period Spectral types
(eclipsing components)		 Comment
AB And Andromeda   10m.40 11m.27 0.87 0.3319 d G5+G5V
S Ant Antlia H.M.Paul, 1891 6m.27 6m.83 0.56 0.6483489 d
44 (i Boö) Boötes   5m.8 6m.4 0.6 0.2678159 d G2V + G2VBoö triple system
TU Boö Boötes   11m.8 12m.5 0.7
VW Cep Cepheus   7m.23 7m.68 0.45 0.278 d G5+K0Ve
WZ Cep Cepheus   11m.4 12m.0 0.6 0.41744 d F5 Possible third companion
ε CrA Corona Australis   4m.74 5m.0 0.26 0.5914264 d
SX Crv Corvus 8m.99 9m.25 0.26 0.32 d F7V + ?
V1191 Cyg Cygnus 10m.82 11m.15 0.33 0.31 d F6V + G5V
XY Leo Leo   9m.45 9m.93 0.48 0.284 d K0V+K0
CE Leo Leo   11m.8 12m.6 0.8 0.303 d
TV Pic Pictor Verschuren, 1987 7m.37 7m.53 0.16 0.85 d
Y Sex Sextans 9m.81 10m.23 0.42 0.42 d Possibly two substellar companions
W UMa Ursa Major   7m.75 8m.48 0.73 0.3336 d F8Vp + F8Vp prototype, possible triple system

References

  1. ↑ Wilson, R. E. (2001). "Binary Star Morphology and the Name Overcontact". Information Bulletin on Variable Stars. 5076: 1. Bibcode:2001IBVS.5076....1W.
  2. ↑ L. Binnendijk, Veroeffentlichungen der Remeis-Sternwarte zu Bamberg, Nr. 40., p. 36, 1965
  3. ↑ Astronomy and Astrophysics, Vol. 426, pp. 1001–1005 (2004)
  4. ↑ "Contact Binaries II". 4 July 2013. Bibcode:1967MmRAS..70..111E. Retrieved 4 July 2013.
  5. ↑ Terrell, Dirk; Gross, John; Cooney, Walter (2012). "A BVRCIC Survey of W Ursae Majoris Binaries". Astronomical Journal. 143: 99. Bibcode:2012AJ....143...99T. arXiv:1202.3111 Freely accessible. doi:10.1088/0004-6256/143/4/99.
  6. 1 2 (visual magnitude, unless marked (B) (= blue) or (p) (= photographic))
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