52 Persei is a suspected triple star[2] system in the northern constellation of Perseus. It has the Bayer designation f Persei, while 52 Persei is the Flamsteed designation.[6] The system is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 4.68.[2] It is located around 600 light years away from the Sun based on parallax, and is drifting closer with a radial velocity of −4.5 km/s.[4]

The variable velocity of this system was reported by W. W. Campbell in 1918. It is a single-lined spectroscopic binary with an orbital period of 4.3 years and an eccentricity of 0.4.[5] The components have a visual magnitude difference of 2.7 and are unresolved by speckle interferometry.[2]

The primary component is an evolved bright giant star with a stellar classification of G5II.[3] It has four[2] times the mass of the Sun and has expanded to 32[1] times the Sun's radius. The star is radiating 531[1] times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,868 K.[1] The secondary is a suspected binary of unknown period, with its components having estimated masses equal to 2.4 and 1.0 times the mass of the Sun.[2] The more massive member of the pair has an estimated spectral class of A2V,[3] matching an A-type main-sequence star.

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