binary star

A binary star is a pair of stars that orbit each other. Double star means the same thing except that it also includes stars that are not orbiting and not close together but happen to be on the same line of sight from Earth, referred to as apparent binary or optical double stars. Binary (or more) star systems are said to be common: the most convincingly cited number I've found is that roughly third of all star systems have two or more stars. They are extremely useful in the study of stellar physics, both to use the orbital dynamics for stellar parameter determination, and for those close enough to interact further, giving additional situations to observe, to infer and test the physics of stellar structure.

A system can have three or more stars, termed a higher-order multiple star system, or sometimes the terms multiple star system and multiple star are used specifically for three or more.

A common classification of binary stars is based on the method by which they were determined to be binary:

• visual binary - separate stars can be seen or photographed.
• eclipsing binary - a periodic variation in luminosity suggesting a star passing in front of its companion.
• spectrum binary - a star whose spectrum looks like the combined spectrum of two stars.
• astrometric binary - measurement of the star's position in the sky over time suggests an orbit-like movement around an unseen companion.
• spectroscopic binary - measurement of the spectrum over time shows an apparent Doppler shift signifying the type of radial motion that orbiting a companion would produce.

Another classification is based upon how close they are and how much they interact:

• compact binary - small orbits: one criteria is that they rotate in five days or less.
• close binary star - similar meaning: close enough to consider their cross-influence and interaction.
• detached binary - sufficiently distant that the stars are (basically) spherical.
• semidetached binary - sufficiently close that one of the stars transfers mass to the other, but not touching.
• contact binary - touching; at minimum, both stars "stretched" by gravity to a contact point.

A binary star's mass ratio (μ) is the ratio of the two masses, i.e., 1 for stars of equal mass. When the total mass can also be determined, e.g., from the orbital period and size, the mass of each star is evident.

Binary stars generally have similar composition (as shown by their spectra), as if they were formed together. Binaries formed together are known as primordial binaries, another sign being aligned rotation axes. A capture requires the coincidence of stars passing close to each other, plus something to change their velocity, such as a third star, or with just two, tidal forces between them (i.e., tidal-capture binaries). The "close pass" is more likely in areas with a very high density of stars such as the center of globular clusters or galaxies.

Given the large range of distances between the stars and the different sizes/spectral types of the individual stars, binary stars show a wide variety and interactions between them produce characteristics unseen in non-binary stars. For example:

• barium star - a star showing unexpected barium absorption lines, often apparently a red giant that previously received mass from a companion carbon star.
• X-ray binary (XRB) or binary X-ray system - includes an accreting neutron star or black hole, whose high gravitational potential energy provides the energy to produce X-rays (through shock). With a strong magnetic field, it might be an X-ray pulsar. These may be low-mass X-ray binaries (LMXB), intermediate-mass X-ray binaries (IMXB), or high-mass X-ray binaries (HMXB or massive X-ray binaries, MXRB) according to the mass of the companion star to the BH/neutron-star. Some are X-ray bursters, with bursts thought to stem from changing levels of accretion, such a transient termed an X-ray burst or X-ray nova. A Be X-ray binary (BeXRB) is a such a binary including a Be star.
• VV Cephei systems - (like VV Cephei) consisting of a giant star and a hot star forming a long-period, interacting eclipsing binary.
• ζ Aurigae systems - (or Zeta Aurigae systems, like the star ζ Aurigae) are analogous to VV Cephei systems but with a different class of giant.
• Algol.
• post-common envelope binary (PCEB).

The commonly-used system for designating the individual stars of a binary/multiple star system consist of adding letters to the star system's designator, with letter "A" for the brightest, "B" for the second brightest, then "C" and so on. For example, the two stars making up Sirius are termed "Sirius A" and "Sirius B". If two are very close and a third is distant, the two close stars might use lower-case suffixes, i.e., "Aa" and "Ab", with the further member called "B".