Astronomy:Omicron Pegasi
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22h 41m 45.39893s[1] |
| Declination | +29° 18′ 27.5542″[1] |
| Apparent magnitude (V) | +4.80[2] |
| Characteristics | |
| Spectral type | A1 IV[3] |
| U−B color index | +0.035[4] |
| B−V color index | −0.013±0.002[2] |
| Astrometry | |
| Radial velocity (Rv) | +8.5±0.1[2] km/s |
| Proper motion (μ) | RA: −0.106[1] mas/yr Dec.: −31.691[1] mas/yr |
| Parallax (π) | 11.4116 ± 0.4055[1] mas |
| Distance | 290 ± 10 ly (88 ± 3 pc) |
| Absolute magnitude (MV) | −0.01[3] |
| Details | |
| Mass | 2.24[5] M☉ |
| Radius | 3.37±0.10[6] R☉ |
| Luminosity | 85±6[6] L☉ |
| Surface gravity (log g) | 3.81±0.04[6] cgs |
| Temperature | 9,600±50[6] K |
| Metallicity [Fe/H] | +0.25±0.09[6] dex |
| Rotational velocity (v sin i) | 6.0±0.2[3] km/s |
| Age | 184[5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
ο Pegasi, Latinized as Omicron Pegasi, is a suspected astrometric binary[8] 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.[2] The distance to this system is approximately 290 light years based on parallax,[1] and it is drifting further away from the Sun with a radial velocity of +8.5 km/s.[2]
The visible component has a stellar classification of A1 IV,[3] 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.[3] Omicron Pegasi is an estimated 184 million years old with 2.24 times the mass of the Sun.[5] It is radiating 85 times the Sun's luminosity from its photosphere at an effective temperature of 9,600 K.[6]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 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 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A
- ↑ 3.0 3.1 3.2 3.3 3.4 Gray, David F. (April 2014). "Precise Rotation Rates for Five Slowly Rotating a Stars". The Astronomical Journal 147 (4): 13. doi:10.1088/0004-6256/147/4/81. 81. Bibcode: 2014AJ....147...81G.
- ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ 5.0 5.1 5.2 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. doi:10.1088/0004-637X/804/2/146. Bibcode: 2015ApJ...804..146D.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 Romanovskaya, A M; Ryabchikova, T A; Pakhomov, Yu V; Korotin, S A; Sitnova, T M (2023-12-11), "Non-LTE abundance analysis of A-B stars with low rotational velocities – II. Do A-B stars with normal abundances exist?", Monthly Notices of the Royal Astronomical Society 526 (3): 3386–3399, doi:10.1093/mnras/stad2862, ISSN 0035-8711.
- ↑ "omi Peg". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=omi+Peg.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
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