Contact binary

In astronomy, a contact binary is a binary star system whose component stars are so close that they touch each other or have merged to share their gaseous envelopes. A binary system whose stars share an envelope may also be called an overcontact binary.[1][2] The term "contact binary" was introduced by astronomer Gerard Kuiper in 1941.[3] Almost all known contact binary systems are eclipsing binaries;[4] eclipsing contact binaries are known as W Ursae Majoris variables, after their type star, W Ursae Majoris.[5]

Artist's rendering of the massive contact binary star VFTS 352, located in the Large Magellanic Cloud

In a contact binary, both stars have filled their Roche lobes, allowing the more massive primary component to transfer both mass and luminosity to the secondary member. As a result, the components in a contact binary often have similar effective temperatures and luminosities, regardless of their respective masses. The rate of energy transfer between the components is dependent on their mass ratio and luminosity ratio. In cases where the stars are in geometric contact but the thermal contact is poor, there can exist wide differences between their respective temperatures.[6]

Contact binaries are not to be confused with common envelopes. Whereas the configuration of two touching stars in a contact binary has a typical lifetime of millions to billions of years, the common envelope is a dynamically unstable phase in binary evolution that either expels the stellar envelope or merges the binary in a timescale of months to years.[7]

See also

• Contact binary (small Solar System body), two asteroids gravitating toward each other until they touch.
• HR 5171, a yellow hypergiant and yellow supergiant contact binary with a third star orbiting further out.
• KIC 9832227, a contact binary and a previous candidate for stellar merger.
• Luminous red nova, e.g. V1309 Scorpii (2008), may result from the merger of a contact binary.
• Thorne–Żytkow object, a type of star wherein a red giant or supergiant contains a neutron star at its core.
• VFTS 352, a massive contact binary in the Tarantula Nebula.

References

1. Darling, David. "binary star". www.daviddarling.info. Retrieved 2019-05-06.
2. Thompson, Michael J. (2006). An Introduction to Astrophysical Fluid Dynamics. London: Imperial College Press. pp. 51–53. ISBN 1-86094-615-1.
3. Kuiper, Gerard P. (1941). "On the Interpretation of β Lyrae and Other Close Binaries". Astrophysical Journal. 93: 133. Bibcode:1941ApJ....93..133K. doi:10.1086/144252.
4. Tassoul, Jean Louis; et al. (2000). Stellar Rotation. Cambridge, UK, New York: Cambridge University Press. p. 231. ISBN 0-521-77218-4.
5. Mullaney, James (2005). Double and Multiple Stars and how to Observe Them. New York, London: Springer. p. 19. ISBN 1-85233-751-6.
6. Csizmadia, Sz.; Klagyivik, P. (November 2004). "On the properties of contact binary stars". Astronomy and Astrophysics. 426: 1001–1005. arXiv:astro-ph/0408049. Bibcode:2004A&A...426.1001C. doi:10.1051/0004-6361:20040430.
7. Ivanova, N.; et al. (2013). "Common envelope evolution: where we stand and how we can move forward". The Astronomy and Astrophysics Review. 21: 59. arXiv:1209.4302. Bibcode:2013A&ARv..21...59I. doi:10.1007/s00159-013-0059-2.