Sigma Pegasi
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 22h 52m 24.07496s[1] |
| Declination | +09° 50′ 08.3791″[1] |
| Apparent magnitude (V) | 5.16[2] + 13.5[3] |
| Characteristics | |
| Spectral type | F6 V[4] or F7 IV[5] + M4 V[3] |
| U−B color index | −0.016[2] |
| B−V color index | +0.486[2] |
| Astrometry | |
| Radial velocity (Rv) | +11.4[6] km/s |
| Proper motion (μ) | RA: +521.04[1] mas/yr Dec.: +42.65[1] mas/yr |
| Parallax (π) | 36.66 ± 0.29 mas[1] |
| Distance | 89.0 ± 0.7 ly (27.3 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.01[7] |
| Details | |
| σ Peg A | |
| Mass | 1.275[6] M☉ |
| Surface gravity (log g) | 3.69[4] cgs |
| Temperature | 6,250[4] K |
| Metallicity [Fe/H] | −0.32[4] dex |
| Rotational velocity (v sin i) | 3[8] km/s |
| Age | 2.71±0.61[9] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
σ Pegasi, Latinised as Sigma Pegasi, is a binary star[3] system in the northern constellation of Pegasus. With a combined apparent visual magnitude of 5.16,[2] it is faintly visible to the naked eye. Based upon an annual parallax shift of 36.66 mas as seen from Earth,[1] the system is located 89 light years distant from the Sun. It has a relatively high proper motion, advancing across the celestial sphere at the rate of 0.524 arcseconds per year.[11]
The primary, component A, is a yellow-white hued F-type main-sequence star with a stellar classification of F6 V.[4] However, Frasca et al. (2009) lists it as a somewhat more evolved F-type subgiant star with a class of F7 IV.[5] At the age of 2.7[9] billion years, it has an inactive chromosphere[4] and is spinning with a leisurely projected rotational velocity of 3 km/s.[8] It has a faint, magnitude 13.23[12] red dwarf companion, designated component B, at an angular separation of 248 arc seconds.[3] The system is most likely (96% chance) a member of the thin disk population of the Milky Way.[6]
References
[edit]- ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
- ^ a b c d Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
- ^ a b c d 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.
- ^ a b c d e f Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–70, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ a b Frasca, A.; et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics, 508 (3): 1313–1330, arXiv:0911.0760, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327, S2CID 118361131.
- ^ a b c Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78, S2CID 118751608.
- ^ Karatas, Y.; Schuster, W. J. (October 2006), "Metallicity and absolute magnitude calibrations for UBV photometry", Monthly Notices of the Royal Astronomical Society, 371 (4): 1793–1812, Bibcode:2006MNRAS.371.1793K, doi:10.1111/j.1365-2966.2006.10800.x.
- ^ a b Takeda, Yoichi; et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F—K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan, 57 (1): 13–25, Bibcode:2005PASJ...57...13T, doi:10.1093/pasj/57.1.13.
- ^ a b Pace, G. (March 2013), "Chromospheric activity as age indicator. An L-shaped chromospheric-activity versus age diagram", Astronomy & Astrophysics, 551: 4, arXiv:1301.5651, Bibcode:2013A&A...551L...8P, doi:10.1051/0004-6361/201220364, S2CID 56420519, L8.
- ^ "49 Peg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-08-10.
{{cite web}}: CS1 maint: postscript (link) - ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ Lépine, Sébastien; Bongiorno, Bethany (2007), "New Distant Companions to Known Nearby Stars. II. Faint Companions of Hipparcos Stars and the Frequency of Wide Binary Systems", The Astronomical Journal, 133 (3): 889–905, arXiv:astro-ph/0610605, Bibcode:2007AJ....133..889L, doi:10.1086/510333, S2CID 16800796.
External links
[edit]- Kaler, James B. (November 6, 2015), "Sigma Pegasi", STARS, University of Illinois, retrieved 2017-08-11.
