Proxima Centauri is a red dwarf star with a mass about 12.
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Proxima Centauri is a red dwarf star with a mass about 12.
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Proxima Centauri is a red dwarf, because it belongs to the main sequence on the Hertzsprung–Russell diagram and is of spectral class M5.
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The measured surface gravity of Proxima Centauri, given as the base-10 logarithm of the acceleration in units of cgs, is 5.
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Red dwarf with the mass of Proxima Centauri will remain on the main sequence for about four trillion years.
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The gravitational influence of Proxima might have stirred up the Alpha Centauri protoplanetary disks.
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Ever since the discovery of Proxima Centauri, it has been suspected to be a true companion of the Alpha Centauri binary star system.
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In 1998, an examination of Proxima Centauri using the Faint Object Spectrograph on board the Hubble Space Telescope appeared to show evidence of a companion orbiting at a distance of about 0.
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Proxima Centauri c is a candidate super-Earth or gas dwarf about 7 Earth masses orbiting at roughly 1.
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An equally accurate parallax determination of Proxima Centauri was made by American astronomer Harold L Alden in 1928, who confirmed Innes's view that it is closer, with a parallax of 0.
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In 1951, American astronomer Harlow Shapley announced that Proxima Centauri is a flare star.
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Proxima Centauri has since been the subject of study by most X-ray observatories, including XMM-Newton and Chandra.
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The probes would perform a fly-by of Proxima Centauri to take photos and collect data of its planets' atmospheric compositions.
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