57 Pegasi

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57 Pegasi
GZPegLightCurve.png
A broadband optical light curve for GZ Pegasi, adapted from Tabur et al. (2009) [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Pegasus
Right ascension 23h 09m 31.45738s [2]
Declination +08° 40′ 37.7636″ [2]
Apparent magnitude  (V)5.105 [3] (4.95 to 5.23) [4]
Characteristics
Evolutionary stage Asymptotic giant branch [5] + main sequence [3]
Spectral type M4IIIa + A3V [3]
U−B color index 1.272 [3]
B−V color index 1.452 [3]
Variable type SRa [4]
Astrometry
Radial velocity (Rv)+14.0±0.9 [6]  km/s
Proper motion (μ)RA: +4.28 [2]   mas/yr
Dec.: −6.29 [2]   mas/yr
Parallax (π)4.17 ± 0.34  mas [2]
Distance 780 ± 60  ly
(240 ± 20  pc)
Absolute magnitude  (MV)−1.83 [7]
Details
Aa
Mass 3 M☉ [8]
2 [5]   M☉
Radius 126+23
−17 [9]   R☉
Luminosity 2,697±311 [9]   L☉
Surface gravity (log g)0.06 [5]   cgs
Temperature 3,707+387
−227 [9]   K
Metallicity [Fe/H]−0.99 [5]   dex
Ab
Mass 1.9 [8]   M☉
Other designations
57 Peg, GZ Peg, BD+07°4981, HD  218634, HIP  114347, HR  8815, SAO  128001, WDS 23095+0841 [10]
Database references
SIMBAD data

57 Pegasi is a variable binary star system in the northern constellation of Pegasus (constellation). It has the variable star designation GZ Pegasi, while 57 Pegasi is the Flamsteed designation. The system is faintly visible to the naked eye as a point of light with an apparent visual magnitude that fluctuates around 5.105. [3] It is located at a distance of approximately 780  light years from the Sun based on parallax, [2] and is drifting further away with a radial velocity of +14 km/s. [6]

The variability of this star was discovered by J. Stebbins and C. M. Huffer in 1930. [11] It was classified as a long-period variable of type Lb in 1974. However, based on a constant period and the shape of the light curve, it was later reclassified as a semiregular variable of type SRa in 1978. [12] It varies in brightness from magnitude 4.95 down to 5.23 with a period of 92.66 days. [4] The spectrum of 57 Peg displays blended features that indicate this is a binary system consisting of an aging red giant star on the asymptotic giant branch [5] with a stellar classification of M4IIIa, and a fainter but hotter A-type main-sequence companion of class A3V. [3] This spectroscopic binary system has poorly constrained orbital elements with an estimated orbital period of 100–500 years. [8]

The red giant primary has been designated as an S-type star that shows enriched levels of s-process elements in its spectrum. However, it does not display significant lines of radioactive technetium-99 in its spectrum, indicating that the s-process elements must have been acquired from a mass transfer event from a formerly asymptotic giant branch companion that had passed through multiple dredge-up events. [5] This would suggest it has a white dwarf as a tertiary companion, but this is incompatible with the data findings. Instead, it might have been misclassified as an S-type star. [8]

There is a magnitude 10.06 visual companion at an angular separation of 32.6″ along a position angle of 198° from the primary, as of 2015. Designated component B, this star was first reported by F. G. W. Struve in 1827. [13]

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<span class="mw-page-title-main">13 Sagittae</span> Star in the constellation Sagitta

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EQ Pegasi is a nearby binary system of two red dwarfs. Both components are flare stars, with spectral types of M4Ve and M6Ve respectively, and a current separation between the components of 5.8 arcseconds. The system is at a distance of 20.4 light-years, and is 950 million years old. The primary star is orbited by one known exoplanet.

<span class="mw-page-title-main">HN Pegasi</span> Star in the constellation Pegasus

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<span class="mw-page-title-main">TW Horologii</span> Star in the constellation Horologium

TW Horologii is a carbon star and semiregular variable in the southern constellation of Horologium, near the eastern constellation border with Reticulum. It has a ruddy hue and, with an apparent visual magnitude that ranges from 5.52 down to 5.95, is visible to the naked eye and one of the brightest carbon stars. Based on parallax measurements, it is located at a distance of approximately 1,370 light years from the Sun. It is drifting further away with a radial velocity of +14 km/s. In the past this star has been considered a member of the open cluster NGC 1252, but this now seems unlikely.

<span class="mw-page-title-main">U Lacertae</span> Binary star in the constellation Lacerta

U Lacertae is a spectroscopic binary star in the constellation Lacerta.

<span class="mw-page-title-main">DY Pegasi</span> Star in the constellation Pegasus

DY Pegasi, abbreviated DY Peg, is a binary star system in the northern constellation of Pegasus. It is a well-studied SX Phoenicis variable star with a brightness that ranges from an apparent visual magnitude of 9.95 down to 10.62 with a period of 1.75 hours. This system is much too faint to be seen with the naked eye, but can be viewed with large binoculars or a telescope. Based on its high space motion and low abundances of heavier elements, it is a population II star system.

<span class="mw-page-title-main">LO Pegasi</span> Star in the constellation Pegasus

LO Pegasi is a single star in the northern constellation of Pegasus that has been the subject of numerous scientific studies. LO Pegasi, abbreviated LO Peg, is the variable star designation. It is too faint to be viewed with the naked eye, having an apparent visual magnitude that ranges from 9.04 down to 9.27. Based on parallax measurements, LO Peg is located at a distance of 79 light years from the Sun. It is a member of the young AB Doradus moving group, and is drifting closer with a radial velocity of −23 km/s.

References

  1. ↑ Tabur, V.; Bedding, T. R.; Kiss, L. L.; Moon, T. T.; Szeidl, B.; Kjeldsen, H. (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 . S2CID   15358380.
  2. 1 2 3 4 5 6 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.
  3. 1 2 3 4 5 6 7 Hackos, W. Jr.; Peery, B. F. Jr. (August 1968), "Spectroscopic binary 57 Pegasi", Astronomical Journal, 73: 504–507, Bibcode:1968AJ.....73..504H, doi:10.1086/110651.
  4. 1 2 3 Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID   125853869.
  5. 1 2 3 4 5 6 Pompéia, L. (September 2009), "Chemical Abundances of the S Star GZ Peg", Publications of the Astronomical Society of Australia, 26 (3): 354–358, arXiv: 0903.1053 , Bibcode:2009PASA...26..354P, doi:10.1071/AS08041, S2CID   15407375.
  6. 1 2 Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington, Carnegie Institution of Washington: 0, Bibcode:1953GCRV..C......0W.
  7. ↑ 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.
  8. 1 2 3 4 Jorissen, A.; et al. (June 2019), "Barium and related stars, and their white-dwarf companions. I. Giant stars", Astronomy & Astrophysics, 626: 28, arXiv: 1904.03975 , Bibcode:2019A&A...626A.127J, doi:10.1051/0004-6361/201834630, S2CID   102351666, A127.
  9. 1 2 3 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.
  10. ↑ "57 Peg", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2021-05-16.
  11. ↑ Tremko, J.; Bakos, G. A. (November 1986), "The semiregular variable 57 Pegasi", Journal of the Royal Astronomical Society of Canada, 80: 230–239, Bibcode:1986JRASC..80..230T.
  12. ↑ Bakos, G. A. (1978), "Spectrographic and Photometric Investigation of 57 Pegasi", Bulletin of the Astronomical Institute of Czechoslovakia, 29: 252, Bibcode:1978BAICz..29..252B.
  13. ↑ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi: 10.1086/323920 , retrieved 2015-07-22
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