astrometric binary oor Portugees

astrometric binary

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binária astrométrica

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They may also be detected by indirect techniques, such as spectroscopy (spectroscopic binaries) or astrometry (astrometric binaries).
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Astrometric binaries are relatively nearby stars which can be seen to wobble around a point in space, with no visible companion.
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Nearby stars often have a relatively high proper motion, so astrometric binaries will appear to follow a wobbly path across the sky.
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Non-visual binaries are stars whose binary status was deduced through more esoteric means, such as occultation (eclipsing binaries), spectroscopy (spectroscopic binaries), or anomalies in proper motion (astrometric binaries).
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At the same time, in 1997, the Hipparcos Catalogue was published revealing Phi Phoenicis to be an astrometric binary with an estimated period of 878 days (circular orbit solution).
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This star is classified with a spectral type of A9/F0III, corresponding to a giant of type A or F. With an estimated radius of 2.7 times the solar radius, it is shining with 19 times the solar luminosity at an effective temperature of 7,280 K. The astrometric observations by the Hipparcos spacecraft detected a significant acceleration in the proper motion of AZ Phoenicis, indicating it is an astrometric binary.
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"An Astrometric Study of the Low-Mass Binary Star Ross 614" (PDF).
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Binary stars are classified into four types according to the way in which they are observed: visually, by observation; spectroscopically, by periodic changes in spectral lines; photometrically, by changes in brightness caused by an eclipse; or astrometrically, by measuring a deviation in a star's position caused by an unseen companion.
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Binary stars are classified into four types according to the way in which they are observed: visually, by observation; spectroscopically, by periodic changes in spectral lines; photometrically, by changes in brightness caused by an eclipse; or astrometrically, by measuring a deviation in a star's position caused by an unseen companion.[4][21] Any binary star can belong to several of these classes; for example, several spectroscopic binaries are also eclipsing binaries. Visual binaries[edit]
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Binary stars are classified into four types according to the way in which they are observed: visually, by observation; spectroscopically, by periodic changes in spectral lines; photometrically, by changes in brightness caused by an eclipse; or astrometrically, by measuring a deviation in a star's position caused by an unseen companion.[5][22] Any binary star can belong to several of these classes; for example, several spectroscopic binaries are also eclipsing binaries. Visual binaries[edit] Main article: Visual binary
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Methods of observationEdit Binary stars are classified into four types according to the way in which they are observed: visually, by observation; spectroscopically, by periodic changes in spectral lines; photometrically, by changes in brightness caused by an eclipse; or astrometrically, by measuring a deviation in a star's position caused by an unseen companion.
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