出典(authority):フリー百科事典『ウィキペディア（Wikipedia）』「2015/10/20 11:17:35」(JST)
| This article needs additional citations for verification. Please help improve this article by adding citations to reliable sources. Unsourced material may be challenged and removed. (February 2015) |
A binary system is a system of two objects in space (usually stars, but also brown dwarfs, planets, galaxies, or asteroids) which are so close that their gravitational interaction causes them to orbit about a common center of mass. Some definitions (e.g. that of double planet, but not that of binary star) require that this center of mass is not located within the interior of either object. A multiple system is like a binary system but consists of three or more objects.
When binary minor planets are similar in size, they may be called "binary companions" instead of referring to the smaller body as a satellite.[1] Good examples of true binary companions are the 90 Antiope and the 79360 Sila–Nunam systems. Pluto and its largest moon Charon are sometimes described as a binary system because the barycenter (center of mass) of the two objects is not inside either of them.[2]
A binary star that has an orbital period of less than 30 years implies that the two system components are less than about 10 AU apart. Because of this proximity, most close binaries are spectroscopic binaries and/or eclipsing binaries. Mass transfer occurs at some stage in most close binaries, profoundly affecting the evolution of the component stars. If the two components are in a close binary and do not fill their Roche lobes, the system is considered a detached binary. In a semidetached binary, one star fills its Roche lobe and mass transfer occurs. In a contact binary, both stars fill their Roche lobes. The evolution of close binaries depends on the initial masses of the two stars and their separation. When the more-massive star evolves into a red giant first and fills its Roche lobe, material will spill through the inner Lagrangian point onto its companion, thereby affecting its companion's evolution. Mass transfer can also alter the separation and orbital period of the binary star.
In binaries that are initially widely separated, material escaping from the Roche lobe of the evolved red giant immerses the system in material, creating a common-envelope binary that contains the core of the red giant (a white dwarf) and the companion star. Friction causes the two components to approach, and thus the orbital period to shorten. The common envelope is ejected and a cataclysmic variable star is left, wherein the mass transfer from the companion to the white dwarf causes the periodic outbursts seen in novae, recurrent novae, dwarf novae, and symbiotic novae.
If one component of a close binary is massive enough, it may become a neutron star or black hole instead of a white dwarf. Such binary systems are observed (see X-ray binary), but often a supernova explosion will blow the system apart into separate single stars.
| Astronomy portal |
全文を閲覧するには購読必要です。 To read the full text you will need to subscribe.
| リンク元 | 「二進法」 |
| 関連記事 | 「system」「binary」 |