| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22 41 45.39893 |
| Declination | +29° 18′ 27.5542″ |
| Apparent magnitude (V) | +4.80 |
| Characteristics | |
| Spectral type | A1 IV |
| U−B color index | +0.035 |
| B−V color index | −0.013±0.002 |
| Astrometry | |
| Radial velocity (Rv) | +8.5±0.1 km/s |
| Proper motion (μ) | RA: −0.106 mas/yr Dec.: −31.691 mas/yr |
| Parallax (π) | 11.4116 ± 0.4055 mas |
| Distance | 290 ± 10 ly (88 ± 3 pc) |
| Absolute magnitude (MV) | −0.01 |
| Details | |
| Mass | 2.24 M☉ |
| Luminosity | 104.24 L☉ |
| Surface gravity (log g) | 3.77±0.14 cgs |
| Temperature | 9,956±338 K |
| Metallicity | 0.0 dex |
| Rotational velocity (v sin i) | 6.0±0.2 km/s |
| Age | 184 Myr |
| Other designations | |
| ο Peg, 43 Pegasi, BD+28°4436, HD 214994, HIP 112051, HR 8641, SAO 90717 | |
| Database references | |
| SIMBAD | data |
ο Pegasi, Latinized as Omicron Pegasi, is a suspected astrometric binary star system in the northern constellation of Pegasus. It is white in hue and visible to the naked eye as a faint point of light with an apparent visual magnitude of +4.80. The distance to this system is approximately 290 light years based on parallax, and it is drifting further away from the Sun with a radial velocity of +8.5 km/s.
The visible component has a stellar classification of A1 IV, matching a subgiant star that has begun to cool, expand and brighten off the main sequence. It has very narrow lines due to a low projected rotational velocity of 6 km/s. The abundances of iron are Sun-like, while it displays an overabundance of heavier elements. Some studies have suggested it is an Am-like star. Omicron Pegasi is an estimated 184 million years old with 2.24 times the mass of the Sun. It is radiating 104 times the Sun's luminosity from its photosphere at an effective temperature of 9,956 K.
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
- ^ Gray, David F. (April 2014). "Precise Rotation Rates for Five Slowly Rotating a Stars". The Astronomical Journal. 147 (4): 13. Bibcode:2014AJ....147...81G. doi:10.1088/0004-6256/147/4/81. S2CID 121928906. 81.
- Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607.
- "omi Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-10.
- Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
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