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57 Persei
Star in the constellation Perseus From Wikipedia, the free encyclopedia
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57 Persei, or m Persei, is a suspected triple star[10] system in the northern constellation of Perseus. It is at the lower limit of visibility to the naked eye, having a combined apparent visual magnitude of 6.08.[2] The annual parallax shift of 16.4 mas provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23[5] km/s and will make perihelion in around 2.6 million years at a distance of roughly 22 ly (6.6 pc).[11]
The primary member, 57 Persei, is a magnitude 6.18,[10] yellow-white hued F-type main-sequence star with a stellar classification of F0 V,[3] indicating it is generating energy by fusing its core hydrogen. It is an estimated 1.6[7] billion years old and is spinning with a projected rotational velocity of 90 km/s.[3] The star has 1.3[7] times the mass of the Sun and is radiating 11 times the Sun's luminosity from its photosphere at an effective temperature of around 6,615 K.[7]
An unseen companion has been identified via slight changes to the proper motion of the primary.[10] The third possible member of the system, designated component B,[12] is a magnitude 6.87 F-type star at an angular separation of 120.13 arc seconds.[10] This star has a different parallax and space velocity than the primary,[13] so it may just be a wide visual companion.[12] There are three other nearby visual companions that are not physically associated with the 57 Persei system.[12]
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