Astronomy:52 Persei
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| 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[1] mas |
| 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 | |
| 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
- ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 2.9 Parsons, Sidney B. (2004). "New and Confirmed Triple Systems with Luminous Cool Primaries and Hot Companions". The Astronomical Journal 127 (5): 2915–2930. doi:10.1086/383546. Bibcode: 2004AJ....127.2915P.
- ↑ 3.0 3.1 3.2 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
- ↑ 4.0 4.1 4.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A.
- ↑ 5.0 5.1 Osawa, K. (May 1957). "The Orbits of the Spectroscopic Binaries 52 Persei and 35 Cygni". Astrophysical Journal 125: 707. doi:10.1086/146344. Bibcode: 1957ApJ...125..707O.
- ↑ 6.0 6.1 "52 Per". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=52+Per.
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