52 Persei
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension 04h 14m 53.32924s[1]
Declination +40° 29′ 01.1973″[1]
Apparent magnitude (V) 4.68[2]
Characteristics
Spectral type G5II + A2V[3]
B−V color index 1.007±0.007[4]
Astrometry
Radial velocity (Rv)−4.50±0.74[4] km/s
Proper motion (μ) RA: +1.249[1] mas/yr
Dec.: −30.506[1] mas/yr
Parallax (π)5.4208 ± 0.2593 mas[1]
Distance600 ± 30 ly
(184 ± 9 pc)
Absolute magnitude (MV)−1.6 / 1.1[2]
Orbit[5]
Period (P)1576.44 days
Eccentricity (e)0.41
Periastron epoch (T)2,425,927.4 JD
Argument of periastron (ω)
(secondary)		66.7°
Semi-amplitude (K1)
(primary)		18.1 km/s
Details
f Per A
Mass4.0[2] M☉
Radius32.40+1.47
−0.83[1] R☉
Luminosity531.1±28.7[1] L☉
Temperature4868+64
−107[1] K
f Per B
Mass2.4[2] M☉
Temperature10,232[2] K
Other designations
f Per, 52 Per, BD+40°912, FK5 2306, GC 5103, HD 26673, HIP 19811, HR 1306, SAO 57000[6]
Database references
SIMBADdata

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.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. 1 2 3 4 5 6 7 8 9 10 Parsons, Sidney B. (2004). "New and Confirmed Triple Systems with Luminous Cool Primaries and Hot Companions". The Astronomical Journal. 127 (5): 2915–2930. Bibcode:2004AJ....127.2915P. doi:10.1086/383546.
  3. 1 2 3 Markowitz, Allan Henry (1969). A Study of Stars Exhibiting Composite Spectra (PhD). The Ohio State University. Bibcode:1969PhDT.........5M. Source: Dissertation Abstracts International, Volume: 30-07, Section: B, page: 3005
  4. 1 2 3 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  5. 1 2 Osawa, K. (May 1957). "The Orbits of the Spectroscopic Binaries 52 Persei and 35 Cygni". Astrophysical Journal. 125: 707. Bibcode:1957ApJ...125..707O. doi:10.1086/146344.
  6. 1 2 "52 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-18.
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