Astronomy:Nu Andromedae

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Short description: Binary star in the constellation Andromeda
Not to be confused with Andromeda V or 5 Andromedae. "ν And" redirects here. For other uses, see Vand.
Nu Andromedae
Diagram showing star positions and boundaries of the Andromeda constellation and its surroundings
10px
Location of ν Andromedae (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Andromeda
Right ascension  00h 49m 48.846s[1]
Declination +41° 04′ 44.08″[1]
Apparent magnitude (V) 4.522[2]
Characteristics
Spectral type B4/5 V[3][4] + F8 V[5]
U−B color index –0.573[2]
B−V color index –0.136[2]
Astrometry
Radial velocity (Rv)–23.9[6] km/s
Proper motion (μ) RA: +21.711[1] mas/yr
Dec.: –18.694[1] mas/yr
Parallax (π)5.7868 ± 0.1857[1] mas
Distance560 ± 20 ly
(173 ± 6 pc)
Absolute magnitude (MV)−1.85[7]
Orbit[5]
Period (P)4.2827 d
Eccentricity (e)0.03
Longitude of the node (Ω)25.°
Periastron epoch (T)18,155.67
Semi-amplitude (K1)
(primary)		71.7 km/s
Semi-amplitude (K2)
(secondary)		101.9 km/s
Details
ν And A
Mass5.9±0.2[3] M☉
Radius3.4[8] R☉
Luminosity1,104[7] L☉
Surface gravity (log g)4.12±0.43[9] cgs
Temperature14,851±396[9] K
Metallicity [Fe/H]+0.14±0.17[9] dex
Rotational velocity (v sin i)20[10] km/s
Age63.1±17.9[3] Myr
Other designations
ν Andromedae, ν And, Nu And, 35 Andromedae, 35 And, BD+40 171, FK5 1021, HD 4727, HIP 3881, HR 226, SAO 36699, PPM 43365[11]
Database references
SIMBADdata

Nu Andromedae is a binary star system in the constellation Andromeda. Its Bayer designation is Latinized from ν Andromedae, and abbreviated Nu And or ν And, respectively. The system has an apparent visual magnitude of 4.5,[2] which is bright enough to be seen with the naked eye. Based on parallax measurements, it is located at a distance of approximately 560 light-years (170 parsecs) from Earth.[1] The pair are drifting closer with a heliocentric radial velocity of –24 km/s.[6] Situated just over a degree to the west of this star is the Andromeda Galaxy.[12]

Nu Andromedae is the prominent blue star in the upper right of this image. At the center is the Andromeda Galaxy.

Nu Andromedae is close spectroscopic binary[3] system with a period of 4.2828 days and a nearly circular orbit.[5] The primary component is a B-type main sequence star with a stellar classification of B5 V.[3] The fainter secondary has a classification of F8 V,[5] which makes it an F-type main sequence star. The pair is about 63 million years old.[3]

The pair have a peculiar velocity of 22.16±0.87 km/s relative to neighboring stars, which doesn't qualify it to be a runaway star system but does suggest it escaped its star cluster of origin. The trajectory indicates it may have left the NGC 6405 cluster some 25 million years ago.[13]

Naming

In Chinese, 奎宿 (Kuí Sù), meaning Legs (asterism), refers to an asterism consisting of ν Andromedae, η Andromedae, 65 Piscium, ζ Andromedae, ε Andromedae, δ Andromedae, π Andromedae, μ Andromedae, β Andromedae, σ Piscium, τ Piscium, 91 Piscium, υ Piscium, φ Piscium, χ Piscium and ψ1 Piscium. Consequently, the Chinese name for ν Andromedae itself is 奎宿七 (Kuí Sù qī, English: the Seventh Star of Legs.)[14]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G.  Gaia EDR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 Oja, T. (April 1983), "UBV photometry of FK4 and FK4 supplement stars", Astronomy and Astrophysics Supplement Series 52: 131–134, Bibcode: 1983A&AS...52..131O. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society 410 (1): 190–200, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T. 
  4. ↑ Nu Andromedae, a blue main-sequence star in Andromeda, http://www.astrostudio.org/xhip.php?hip=3881, retrieved 18 August 2014. 
  5. ↑ 5.0 5.1 5.2 5.3 Pourbaix, D. et al. (September 2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy and Astrophysics 424 (2): 727–732, doi:10.1051/0004-6361:20041213, Bibcode: 2004A&A...424..727P. 
  6. ↑ 6.0 6.1 Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.), Bibcode: 1953GCRV..C......0W. 
  7. ↑ 7.0 7.1 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  8. ↑ Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics 367 (2): 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P. 
  9. ↑ 9.0 9.1 9.2 Koleva, M.; Vazdekis, A. (February 2012), "Stellar population models in the UV. I. Characterisation of the New Generation Stellar Library", Astronomy & Astrophysics 538: A143, doi:10.1051/0004-6361/201118065, Bibcode: 2012A&A...538A.143K. 
  10. ↑ Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal 573 (1): 359–365, doi:10.1086/340590, Bibcode: 2002ApJ...573..359A. 
  11. ↑ "35 And -- Star". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=35+And+--+Star. 
  12. ↑ Mollise, Rod (2006), The Urban Astronomer's Guide: A Walking Tour of the Cosmos for City Sky Watchers, Patrick Moore's Practical Astronomy Series, Springer, p. 178, ISBN 1846282160, https://books.google.com/books?id=Z0mvZk0s_TMC&pg=PA178. 
  13. ↑ Bhat, A. et al. (July 2022), "The origin of early-type runaway stars from open clusters", Astronomy & Astrophysics 663: id. A39, doi:10.1051/0004-6361/202142993, Bibcode: 2022A&A...663A..39B. 
  14. ↑ Script error: The function "in_lang" does not exist. AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 19 日



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