| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22 26 37.37059 |
| Declination | +04° 23′ 37.6056″ |
| Apparent magnitude (V) | 5.76 |
| Characteristics | |
| Spectral type | F7V or F8IV−V + K4 |
| B−V color index | 0.519±0.005 |
| Astrometry | |
| Radial velocity (Rv) | −13.5±0.2 km/s |
| Proper motion (μ) | RA: +307.781 mas/yr Dec.: +47.533 mas/yr |
| Parallax (π) | 24.9028 ± 0.1794 mas |
| Distance | 131.0 ± 0.9 ly (40.2 ± 0.3 pc) |
| Absolute magnitude (MV) | 2.85 |
| Orbit | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | 929.91±0.46 d |
| Semi-major axis (a) | 9.5±0.3" (≥58.24±0.65 Gm) |
| Eccentricity (e) | 0.4358±0.0062 |
| Inclination (i) | 94.0±5.1° |
| Longitude of the node (Ω) | 101.6±4.6° |
| Periastron epoch (T) | 53,293.9±3.2 HJD |
| Argument of periastron (ω) (secondary) | 188.5±1.1° |
| Semi-amplitude (K1) (primary) | 5.060±0.054 km/s |
| Details | |
| Aa | |
| Mass | 1.33 M☉ |
| Radius | 2.25+0.07 −0.08 R☉ |
| Luminosity | 6.7±0.1 L☉ |
| Surface gravity (log g) | 3.92 cgs |
| Temperature | 6,200+110 −100 K |
| Metallicity | −0.04±0.02 dex |
| Rotational velocity (v sin i) | 8.4±1.0 km/s |
| Age | 3.22 Gyr |
| Ab | |
| Mass | 0.29 M☉ |
| Other designations | |
| BU 290, BD+03°4705, GJ 9782, HD 212754, HIP 110785, HR 8548, SAO 127529, WDS J22266+0424, BU 290 | |
| Database references | |
| SIMBAD | data |
34 Pegasi is a triple star system in the northern constellation of Pegasus. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.76. The system is located at a distance of 131 light years from the Sun based on parallax, but is drifting closer with a radial velocity of −13.5 km/s. It has been catalogued as a member of the Hyades Supercluster, although its membership status remains doubtful.
The innermost system is a single-lined spectroscopic binary with an orbital period of 2.55 years and an eccentricity of 0.44. The orbital plane of this pair is being viewed nearly edge-on, and has an angular semimajor axis of 9.5″. A third member of the system has a poorly-constrained 420 year orbit around the main pair. This star was discovered by Burnham in 1874, and the discovery code BU 290 was given to the double. As of 2015, it lies at an angular separation of 3.90±0.02 along a position angle of 226.2°±0.8° from the inner system.
The primary member, component Aa, is an F-type main-sequence star that is starting to evolve off the main sequence, with stellar classifications of F7V or F8IV−V, depending on the source. It is around three billion years old and is spinning with a projected rotational velocity of 8 km/s, with a measured rotation period of 12 days. The star has 1.3 times the mass of the Sun and 2.25 times the Sun's radius. It is radiating 6.7 times the luminosity of the Sun from its photosphere at an effective temperature of 6,200 K.
The secondary companion to the primary, component Ab, is most likely a red dwarf star with around 29% of the mass of the Sun. The tertiary member, component B, has 53% of the Sun's mass and a class of around K4.
References
- ^ 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.
- ^ 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.
- ^ Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
- ^ Willmarth, Daryl W.; et al. (August 2016), "Spectroscopic Orbits for 15 Late-type Stars" (PDF), The Astronomical Journal, 152 (2): 13, Bibcode:2016AJ....152...46W, doi:10.3847/0004-6256/152/2/46, S2CID 53648490, 46.
- ^ Griffin, R. F. (February 2010), "Spectroscopic binary orbits from photoelectric radial velocities - Paper 210: Psi2 Aurigae and 34 Pegasi", The Observatory, 130 (1): 17–32, Bibcode:2010Obs...130...17G.
- ^ Luck, R. Earle (January 2017), "Abundances in the Local Region II: F, G, and K Dwarfs and Subgiants", The Astronomical Journal, 153 (1): 19, arXiv:1611.02897, Bibcode:2017AJ....153...21L, doi:10.3847/1538-3881/153/1/21, S2CID 119511744, 21.
- ^ Roberts, Lewis C. Jr.; et al. (March 2017), "Continued Kinematic and Photometric Investigations of Hierarchical Solar-type Multiple Star Systems", The Astronomical Journal, 153 (3): 7, arXiv:1701.05865, Bibcode:2017AJ....153..100R, doi:10.3847/1538-3881/153/3/100, S2CID 119013557, 100.
- "34 Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-01.
- Eggen, Olin J. (October 1992), "The Hyades Supercluster in FK5", Astronomical Journal, 104: 1482, Bibcode:1992AJ....104.1482E, doi:10.1086/116333.
- Tokovinin, Andrei; Horch, Elliott P. (November 2016), "Speckle Interferometry of Secondary Components in Nearby Visual Binaries", The Astronomical Journal, 152 (5): 7, arXiv:1608.06586, Bibcode:2016AJ....152..116T, doi:10.3847/0004-6256/152/5/116, S2CID 119270753, 116.
- Tokovinin, Andrei (2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 87, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, S2CID 56066740.
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