Contact binary: Difference between revisions
imported>Praemonitus →See also: Add link |
imported>DreamRimmer bot II m Standardise list-defined references format (bot) |
||
| Line 20: | Line 20: | ||
==References== | ==References== | ||
<references> | |||
<ref name=Csizmadia2004>{{cite journal | <ref name=Csizmadia2004>{{cite journal | ||
| Line 69: | Line 69: | ||
| title=Common envelope evolution: where we stand and how we can move forward | | title=Common envelope evolution: where we stand and how we can move forward | ||
| display-authors=1 | journal=The Astronomy and Astrophysics Review | | display-authors=1 | journal=The Astronomy and Astrophysics Review | ||
| year=2013 | volume=21 | | | year=2013 | volume=21 | article-number=59 | ||
| bibcode=2013A&ARv..21...59I | arxiv=1209.4302 | | bibcode=2013A&ARv..21...59I | arxiv=1209.4302 | ||
| doi=10.1007/s00159-013-0059-2 }}</ref> | | doi=10.1007/s00159-013-0059-2 }}</ref> | ||
| Line 82: | Line 82: | ||
| doi=10.1086/144252 |doi-access=free}}</ref> | | doi=10.1086/144252 |doi-access=free}}</ref> | ||
</references> | |||
[[Category:Binary stars|*]] | [[Category:Binary stars|*]] | ||
Latest revision as of 15:40, 18 November 2025
Template:Short description Script error: No such module "about".
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 archetype star, W Ursae Majoris.[5]
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 previously thought to be a contact binary.
- Interacting binary star
- 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.
- MY Camelopardalis, a contact binary that is already sharing an atmosphere with each other
- 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
- ↑ Script error: No such module "citation/CS1".
- ↑ Script error: No such module "citation/CS1".
- ↑ Script error: No such module "Citation/CS1".
- ↑ Script error: No such module "citation/CS1".
- ↑ Script error: No such module "citation/CS1".
- ↑ Script error: No such module "Citation/CS1".
- ↑ Script error: No such module "Citation/CS1".