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m Mass, radius and luminosity of the Luyten 726-8 B in the table had the erroneous title of Luyten 726-8 A. |
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[[File:Toronto Andrew Posa 01.jpg|thumb|left|''UV Ceti'' by Andrew Posa (1982)]]
Soon after{{When|date=January 2012}} the discovery of Luyten 726-8A, the slightly brighter companion star Luyten 726-8B was discovered. Like Luyten 726-8A, this star was also found to be variable and given the variable star designation '''UV Ceti'''.<ref name=UV>{{cite web | url=http://www.sai.msu.su/gcvs/cgi-bin/search.cgi?search=UV+Cet | title=Query= UV Cet | publisher=[[Centre de Données astronomiques de Strasbourg]] | work=[[General Catalogue of Variable Stars]] | accessdate=2009-12-16}}</ref> Although UV Ceti was not the first flare star discovered, it is the most prominent example of such a star,
In approximately 31,500 years, Luyten 726-8 will have a close encounter with [[Epsilon Eridani]] at the minimal distance of about 0.93 [[ly]]. Luyten 726-8 can penetrate a conjectured [[Oort cloud]] about Epsilon Eridani, which may gravitationally [[Perturbation (astronomy)|perturb]] some long-period [[comet]]s. The duration of mutual transit of two star systems within 1 [[ly]] from each other is about 4,600 years.<ref>{{cite web
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