Beta Pegasi
 Location of β Pegasi (circled) | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Pegasus |
| Right ascension | 23h 03m 46.45746s[1] |
| Declination | +28° 04′ 58.0336″[1] |
| Apparent magnitude (V) | 2.42[2] |
| Characteristics | |
| Spectral type | M2.3 II-III[3] |
| U−B color index | +1.96[2] |
| B−V color index | +1.67[2] |
| Variable type | Semi-regular[4] |
| Astrometry | |
| Radial velocity (Rv) | +8.7[5] km/s |
| Proper motion (μ) | RA: +187.65[1] mas/yr Dec.: +136.93[1] mas/yr |
| Parallax (π) | 16.64 ± 0.15[1] mas |
| Distance | 196 ± 2 ly (60.1 ± 0.5 pc) |
| Absolute magnitude (MV) | -1.49 |
| Details | |
| Mass | 2.1[6] M☉ |
| Radius | 95[7] R☉ |
| Surface gravity (log g) | 1.20[8] cgs |
| Temperature | 3,689[8] K |
| Metallicity [Fe/H] | –0.11[8] dex |
| Rotational velocity (v sin i) | 9.7[9] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Beta Pegasi (β Peg, β Pegasi) is a star in the constellation Pegasus. The apparent visual magnitude of this star averages 2.42, making it the second brightest star in the constellation after Epsilon Pegasi. Its traditional name is Scheat,[10] a name that has also been used for Delta Aquarii. According to Richard H. Allen, this name comes from the Arabic Al Sā'id for 'the upper arm', or from Sa'd. Arabian astronomers named it Mankib al Faras, meaning the "Horse's shoulder". It forms the upper right corner of the Great Square of Pegasus,[10] a prominent rectangular asterism.
Based upon parallax measurements, Beta Pegasi is located about 196 light-years (60 parsecs) from the Earth.[1] It is unusual among bright stars in having a relatively cool surface temperature compared to stars like the Sun.[7] This star has a stellar classification of M2.3 II-III,[3] which indicates the spectrum has characteristics partway between a bright giant and a giant star. It has expanded until it is some 95 times as large, and has a total luminosity of 1500 times that of the Sun.[7] The effective temperature of the star's outer envelope is about 3,700 K,[8] giving the star the characteristic orange-red hue of an M-type star.[11] The photosphere is sufficiently cool for molecules of titanium oxide to form.[12]
Beta Pegasi is a semi-regular variable with a period of 43.3 days[4] and a brightness that varies from magnitude +2.31 to +2.74.[13] It is losing mass at a rate at or below 10–8 times the Sun's mass per year, which is creating an expanding shell of gas and dust with a radius of about 3,500 times the Sun's radius (16 Astronomical Units).[14]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 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
- ↑ 2.0 2.1 2.2 Johnson, H. L. et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99). Bibcode:1966CoLPL...4...99J.
- ↑ 3.0 3.1 3.2 "V* bet Peg -- Pulsating variable Star", SIMBAD (Centre de Données astronomiques de Strasbourg), retrieved 2010-01-05
- ↑ 4.0 4.1 Tabur, V. et al. (December 2009), "Long-term photometry and periods for 261 nearby pulsating M giants", Monthly Notices of the Royal Astronomical Society 400 (4): 1945–1961, arXiv:0908.3228, Bibcode:2009MNRAS.400.1945T, doi:10.1111/j.1365-2966.2009.15588.x
- ↑ Wilson, Ralph Elmer (1953), General Catalogue of Stellar Radial Velocities, Washington: Carnegie Institution of Washington, Bibcode:[http://adsabs.harvard.edu/abs/1953QB901.W495..... 1953QB901.W495.....]
- ↑ Tsuji, Takashi (May 2007), "Isotopic abundances of Carbon and Oxygen in Oxygen-rich giant stars", in Kupka, F.; Roxburgh, I.; Chan, K., Convection in Astrophysics, Proceedings of IAU Symposium #239 held 21-25 August, 2006 in Prague, Czech Republic, pp. 307–310, arXiv:astro-ph/0610180, Bibcode:2007IAUS..239..307T, doi:10.1017/S1743921307000622
- ↑ 7.0 7.1 7.2 Kaler, James B. (May 22, 2009), "SCHEAT (Beta Pegasi)", Stars (University of Illinois), retrieved 2010-01-05
- ↑ 8.0 8.1 8.2 8.3 Soubiran, C. et al. (2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788
- ↑ Massarotti, Alessandro et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209
- ↑ 10.0 10.1 Allen, Richard Hinckley (1899), Star Names: Their Lore and Meaning, New York, NY: Dover Publications Inc., p. 325, ISBN 0-486-21079-0
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16
- ↑ Gavin, M. (February 1996), "Stellar spectroscopy with CCDs - some preliminary results", Journal of the British Astronomical Association 106 (1): 11–15, Bibcode:1996JBAA..106...11G
- ↑ "Query= bet Peg", General Catalogue of Variable Stars (Centre de Données astronomiques de Strasbourg), retrieved 2010-01-05
- ↑ Mauron, N.; Caux, E. (November 1992), "K I/Na I scattering observations in circumstellar envelopes - Alpha(1) Herculis, Omicron Ceti, TX PISCIUM and Beta Pegasi", Astronomy and Astrophysics 265 (2): 711–725, Bibcode:1992A&A...265..711M. Solar Radius = 0.0046491 AU.
Coordinates: 
23h 03m 46.458s, +28° 04′ 58.04″
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