Astronomy:Pi1 Cygni

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Short description: Star in the constellation Cygnus


For other stars with this Bayer designation, see π Cygni.
Pi1 Cygni
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cygnus
Right ascension  21h 42m 05.66458s[1]
Declination +51° 11′ 22.6415″[1]
Apparent magnitude (V) 4.66[2]
Characteristics
Spectral type B3 IV[3]
B−V color index −0.11[2]
Astrometry
Proper motion (μ) RA: +5.29[1] mas/yr
Dec.: −1.78[1] mas/yr
Parallax (π)1.89 ± 0.15[1] mas
Distance1,700 ± 100 ly
(530 ± 40 pc)
Absolute magnitude (MV)−3.91[4]
Details
Mass10.1±0.1[3] M☉
Radius15.1[5] R☉
Luminosity6,433[5] L☉
Surface gravity (log g)4.08[6] cgs
Temperature14,863[6] K
Rotational velocity (v sin i)55[7] km/s
Age25.1±0.8[3] Myr
Other designations
Azelfafage, π1 Cyg, 80 Cyg, BD+50°3410, FK5 3733, HD 206672, HIP 107136, HR 8301, SAO 33665[8]
Database references
SIMBADdata
Cygnus (Star is on the far right)

Pi1 Cygni, also named Azelfafage /əˈzɛlfəfeɪdʒ/, is a star in the northern constellation of Cygnus. It is visible to the naked eye, having a combined apparent visual magnitude of 4.66.[2] The distance to this system can be roughly gauged by its annual parallax shift of 1.89 mas,[1] which yields a separation of around 1,700 light years from the Sun, give or take a hundred light years.

Nomenclature

π1 Cygni (Latinised to Pi1 Cygni, abbreviated Pi1 Cyg, π1 Cyg) is the star's Bayer designation. The designations of the two components as Pi1 Cygni A and B derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[9]

It bore the traditional name Azelfafage, derived from the Arabic al-sulaḥfāh, the tortoise, originally a name for Lyra that was misattributed to a star in Cygnus.[10][11] R. H. Allen's 1899 book Star Names incorrectly[10] states that the name is derived from ظلف الفرس Dhilf al-faras meaning "the horse track" or (probably) ذيل الدجاجة Dhail al-dajājah meaning "the tail of the hen".[12] In 2016, the IAU organized a Working Group on Star Names (WGSN)[13] to catalogue and standardize proper names for stars. The WGSN approved the name Azelfafage for Pi1 Cygni on 12 September 2016 and it is now so included in the List of IAU-approved Star Names.[14]

In Chinese, 螣蛇 (Téng Shé), meaning Flying Serpent, refers to an asterism consisting of Pi1 Cygni, Alpha Lacertae, 4 Lacertae, Pi2 Cygni, HD 206267, Epsilon Cephei, Beta Lacertae, Sigma Cassiopeiae, Rho Cassiopeiae, Tau Cassiopeiae, AR Cassiopeiae, 9 Lacertae, 3 Andromedae, 7 Andromedae, 8 Andromedae, Lambda Andromedae, Kappa Andromedae, Psi Andromedae and Iota Andromedae. Consequently, the Chinese name for Pi1 Cygni itself is 螣蛇四 (Téng Shé sì, English: the Fourth Star of Flying Serpent).[15]

Properties

Pi1 Cygni has been described as a single-lined spectroscopic binary with a close, circular orbit, having a period of just 26.33 days.[16] However, a 2020 paper finds no radial velocity variations on the timescale of the published orbit.[17]

The primary, visible, star is a somewhat evolved B-type subgiant star with a stellar classification of B3 IV.[3] It has an estimated 10 times the mass of the Sun and around 5.6[18] times the Sun's radius. The star radiates 16,538[19] times the solar luminosity from its outer atmosphere at an effective temperature of roughly 18,360 K.[2] It is about 25[3] million years old and is spinning with a projected rotational velocity of 55 km/s.[7]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 Soubiran, C. et al. (June 2010), "The PASTEL catalogue of stellar parameters", Astronomy and Astrophysics 515: A111, doi:10.1051/0004-6361/201014247, Bibcode: 2010A&A...515A.111S. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Tetzlaff, N. et al. (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. ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  5. ↑ 5.0 5.1 McDonald, I.; Zijlstra, A. A.; Watson, R. A. (2017). "Fundamental parameters and infrared excesses of Tycho-Gaia stars". Monthly Notices of the Royal Astronomical Society 471 (1): 770. doi:10.1093/mnras/stx1433. Bibcode: 2017MNRAS.471..770M. 
  6. ↑ 6.0 6.1 Cardiel, Nicolás; Zamorano, Jaime; Bará, Salvador; Sánchez De Miguel, Alejandro; Cabello, Cristina; Gallego, Jesús; García, Lucía; González, Rafael et al. (2021). "Synthetic RGB photometry of bright stars: Definition of the standard photometric system and UCM library of spectrophotometric spectra". Monthly Notices of the Royal Astronomical Society 504 (3): 3730. doi:10.1093/mnras/stab997. Bibcode: 2021MNRAS.504.3730C. 
  7. ↑ 7.0 7.1 Strom, Stephen E. et al. (2005), "B Star Rotational Velocities in h and χ Persei: A Probe of Initial Conditions during the Star Formation Epoch?", The Astronomical Journal 129 (2): 809–828, doi:10.1086/426748, Bibcode: 2005AJ....129..809S. 
  8. ↑ "pi.01 Cyg -- Spectroscopic binary", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=pi01+Cyg, retrieved 2017-02-19. 
  9. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  10. ↑ 10.0 10.1 Kunitzsch, P. (March 1979). "A Note on Star Names - Especially Arabic - and Their Literature". Quarterly Journal of the Royal Astronomical Society 20: 478. Bibcode: 1979QJRAS..20..478K. 
  11. ↑ "IAU Catalog of Star Names". https://exopla.net/star-names/modern-iau-star-names/. 
  12. ↑ p. 197, Star-names and Their Meanings, Richard Hinckley Allen, New York, G. E. Stechert, 1899.
  13. ↑ IAU Working Group on Star Names (WGSN), International Astronomical Union, https://www.iau.org/science/scientific_bodies/working_groups/280/, retrieved 22 May 2016. 
  14. ↑ "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. 
  15. ↑ 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 7 月 7 日
  16. ↑ Pourbaix, D. et al. (2004), "SB9: The ninth catalogue of spectroscopic binary orbits", Astronomy & Astrophysics 424 (2): 727–732, doi:10.1051/0004-6361:20041213, Bibcode: 2004A&A...424..727P. 
  17. ↑ Heyne, T.; Mugrauer, M.; Bischoff, R.; Wagner, D.; Hoffmann, S.; Lux, O.; Munz, V.; Geymeier, M. et al. (2020). "Spectroscopic characterization of nine binary star systems as well as HIP 107136 and HIP 107533". Astronomische Nachrichten 341 (1): 99. doi:10.1002/asna.202013683. Bibcode: 2020AN....341...99H. 
  18. ↑ Pasinetti Fracassini, L. E. et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics 367 (2): 521–524, doi:10.1051/0004-6361:20000451, Bibcode: 2001A&A...367..521P. 
  19. ↑ Hohle, M. M. et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten 331 (4): 349, doi:10.1002/asna.200911355, Bibcode: 2010AN....331..349H. 



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