Star in the constellation Perseus
! style="text-align: center; background-color: #FFFFC0;" colspan="2" | Observation dataEpoch J2000      Equinox J2000
! style="text-align:left" | Constellation
! style="text-align:left" | Right ascension
! style="text-align:left" | Declination
! style="text-align:left" | Apparent magnitude (V)
! style="background-color: #FFFFC0; text-align: center;" colspan="2"| Characteristics
! style="text-align:left" | Spectral type
! style="text-align:left" | U−B 
! style="text-align:left" | B−V 
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57 Persei, or m Persei, is a suspected triple star 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. The annual parallax shift of provides a distance measure of 199 light years. 57 Persei is moving closer to the Sun with a radial velocity of about −23 km/s and will make perihelion in around 2.6 million years at a distance of roughly .
The primary member, 57 Persei, is a magnitude 6.18, yellow-white hued F-type main-sequence star with a stellar classification of F0 V, indicating it is generating energy by fusing its core hydrogen. It is an estimated 1.6 billion years old and is spinning with a projected rotational velocity of 90 km/s. The star has 1.3 times the mass of the Sun and is radiating 11 times the Sun's luminosity from its photosphere at an effective temperature of around .
An unseen companion has been identified via slight changes to the proper motion of the primary. The third possible member of the system, designated component B, is a magnitude 6.87 F-type star at an angular separation of 120.13 arc seconds. This star has a different parallax and space velocity than the primary, so it may just be a wide visual companion. There are three other nearby visual companions that are not physically associated with the 57 Persei system.
References.
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