“binary star”的概念、定义、翻译、参考文献-科学参考

binary star

Astronomy

A pair of stars bound together by their mutual gravitation, and orbiting their common centre of mass. Such a system is distinct from an optical double, which is not gravitationally bound.
A visual binary is resolved visually or photographically, whereas an astrometric binary is detectable by irregularities in the proper motion of the one visible star or the photocentre (2). Direct evidence for a companion is provided by the eclipses in an eclipsing binary, and by the Doppler shift of spectral lines in a spectroscopic binary.
The orbital periods of binaries range from minutes to thousands of years. In a close binary, the separation is comparable to the diameter of the stars. Such systems are subdivided according to the amount by which each component fills its Roche lobe, giving rise to detached, semidetached, and contact binaries. The last two categories include interacting binaries, in which mass transfer occurs. Many binaries are also variable stars, the most notable being the various forms of cataclysmic binary, Type I supernovae, and certain variable X-ray sources.

Space Exploration

One of a pair of stars moving in orbit around their common centre of mass. Observations show that most stars are binary, or even multiple; an example is the nearest star system to the Sun, Rigil Kent (Alpha Centauri). A spectroscopic binary is a binary in which two stars are so close together that they cannot be seen separately, but their separate light spectra can be distinguished by a spectroscope. Another type is the eclipsing binary, a double star in which the two stars periodically pass in front of each other as seen from Earth. When one star crosses in front of the other, the total light received on Earth from the two stars declines. The first eclipsing binary to be noticed was Algol, in 1670, by Italian astronomer Geminiano Montanari.
The binary system Rigil Kent, for example, consists of a star almost identical to the Sun with another star about a third as bright closer to it than Neptune is to the Sun (that is, closer than 4.4 billion km). Each of these stars appears to describe an ellipse about the other in about 80 years. A third, much fainter star, Proxima Centauri, is too far away to disturb their mutual orbit appreciably.
The study of binary star systems has provided the only reliable information about the masses of stars. For a few stars it has also yielded direct measures of their dimensions, shapes, and effective temperatures.

单词	binary star
释义	binary star Astronomy A pair of stars bound together by their mutual gravitation, and orbiting their common centre of mass. Such a system is distinct from an optical double, which is not gravitationally bound. A visual binary is resolved visually or photographically, whereas an astrometric binary is detectable by irregularities in the proper motion of the one visible star or the photocentre (2). Direct evidence for a companion is provided by the eclipses in an eclipsing binary, and by the Doppler shift of spectral lines in a spectroscopic binary. The orbital periods of binaries range from minutes to thousands of years. In a close binary, the separation is comparable to the diameter of the stars. Such systems are subdivided according to the amount by which each component fills its Roche lobe, giving rise to detached, semidetached, and contact binaries. The last two categories include interacting binaries, in which mass transfer occurs. Many binaries are also variable stars, the most notable being the various forms of cataclysmic binary, Type I supernovae, and certain variable X-ray sources. Space Exploration One of a pair of stars moving in orbit around their common centre of mass. Observations show that most stars are binary, or even multiple; an example is the nearest star system to the Sun, Rigil Kent (Alpha Centauri). A spectroscopic binary is a binary in which two stars are so close together that they cannot be seen separately, but their separate light spectra can be distinguished by a spectroscope. Another type is the eclipsing binary, a double star in which the two stars periodically pass in front of each other as seen from Earth. When one star crosses in front of the other, the total light received on Earth from the two stars declines. The first eclipsing binary to be noticed was Algol, in 1670, by Italian astronomer Geminiano Montanari. The binary system Rigil Kent, for example, consists of a star almost identical to the Sun with another star about a third as bright closer to it than Neptune is to the Sun (that is, closer than 4.4 billion km). Each of these stars appears to describe an ellipse about the other in about 80 years. A third, much fainter star, Proxima Centauri, is too far away to disturb their mutual orbit appreciably. The study of binary star systems has provided the only reliable information about the masses of stars. For a few stars it has also yielded direct measures of their dimensions, shapes, and effective temperatures.
随便看	Metternich, Klemens Wenzel Nepomuk Lothar, Prince of Metternich-Winneburg-Beilstein (1773–1859) Meudon Observatory Mexican Revolution (1910–40) Mexican–American War (1846–48) Mexico Meyer group Meyerhof, Otto Fritz Meyer, Julius Lothar Meyer, Karl Meyer, Viktor (1848–97) Mečiar, Vladimir (1942–) MF MFCC MFLOPS Mflops MFM M-fold Mg# MGA mgf MGLAB MHC MHC class II protein MHC class I protein MHD