Alpha Trianguli Australis
Epoch J2000 Equinox J2000
|Right ascension||16h 48m 39.89508s|
|Declination||–69° 01′ 39.7626″|
|Apparent magnitude (V)||1.91|
|Spectral type||K2 IIb-IIIa|
|U−B color index||+1.56|
|B−V color index||+1.44|
|Radial velocity (Rv)||–3.3 km/s|
|Proper motion (μ)||RA: 17.99 mas/yr
Dec.: –31.58 mas/yr
|Parallax (π)||8.35 ± 0.15 mas|
|Distance||391 ± 7 ly
(120 ± 2 pc)
|Absolute magnitude (MV)||–3.68|
|Surface gravity (log g)||1.5 cgs|
|Metallicity [Fe/H]||–0.06 dex|
|Age||4.8 × 107 years|
Alpha Trianguli Australis (α TrA, α Trianguli Australis) is the brightest star in the southern circumpolar constellation Triangulum Australe, forming an apex of a triangle with Beta and Gamma Trianguli Australis that gives the constellation its name (Latin for southern triangle). This star has the traditional name Atria, which is merely a contraction of its Bayer designation. In traditional Chinese it is called 三角形三 (Mandarin: sān jiǎo xín sān), the Third Star of the Triangle.
Alpha Trianguli Australis is a bright giant star with an apparent magnitude of +1.91. Based upon parallax measurements, this star is located roughly 391 light-years (120 parsecs) distant from the Earth. The estimated age of the star is 48 million years old; sufficiently old for a massive star to evolve away from the main sequence and expand into a giant. It has a mass roughly seven times the mass of the Sun, but is emitting about 5,500 times the Sun's luminosity. The effective temperature of the star's outer envelope is 4,150 K, which gives it the characteristic orange hue of a K-type star. With a diameter 130 times that of our sun, it would almost reach the orbit of Venus if placed at the centre of our solar system. The proper name Atria is a contraction of its Bayer designation.
There is evidence that Atria may be a binary star. It displays unusual properties for a star of its class, including stellar flares and a higher than normal emission of X-rays. These can be explained by a young, magnetically active companion with a stellar classification of about G0 V. Such a star would have a mass similar to the Sun, with an orbital period of at least 130 years. Young, G-type stars have a high temperature corona and frequently emit flares causing sudden increases in luminosity. The pair may be separated by about 50 Astronomical Units.
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