52 Persei

52 Persei

Observation data Epoch J2000      Equinox J2000
Constellation	Perseus
Right ascension	04^h 14^m 53.32924^s[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]
Distance	600 ± 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
Mass	4.0[2] M☉
Radius	32.40+1.47 −0.83[1] R☉
Luminosity	531.1±28.7[1] L☉
Temperature	4868+64 −107[1] K
f Per B
Mass	2.4[2] M☉
Temperature	10,232[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
SIMBAD	data

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. 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. 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. 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. 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. 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. "52 Per". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-18.