33 Cygni

33 Cygni is a single[7] star located 159 light years away in the northern constellation Cygnus. Its is visible to the naked eye as a white-hued star with an apparent visual magnitude of 4.28.[2] The star is moving closer to the Earth with a heliocentric radial velocity of −16 km/s.[5] Eggen (1995) listed it as a proper motion candidate for membership in the IC 2391 supercluster.[9]

33 Cygni
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension  20h 13m 23.86661s[1]
Declination +56° 34′ 03.7999″[1]
Apparent magnitude (V) 4.28[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A3 IV–Vn[4]
B−V color index 0.114±0.001[2]
Astrometry
Radial velocity (Rv)−16.13±2.53[5] km/s
Proper motion (μ) RA: +61.82[1] mas/yr
Dec.: +82.18[1] mas/yr
Parallax (π)20.48 ± 0.12[1] mas
Distance159.3 ± 0.9 ly
(48.8 ± 0.3 pc)
Absolute magnitude (MV)0.84[2]
Details[3]
Mass2.33±0.01 M☉
Radius2.76[6] R☉
Luminosity44.3±1.0 L☉
Temperature8,395+97
−96 K
Rotational velocity (v sin i)243 km/s
Age400[7] Myr
Other designations
33 Cyg, BD+56°2376, FK5 758, HD 192696, HIP 99655, HR 7740, SAO 32378, WDS J20145+3648A[8]
Database references
SIMBADdata

This star has a stellar classification of A3 IV–Vn,[4] showing a spectrum with traits intermediate between an A-type main-sequence star and an evolving subgiant star. The 'n' suffix indicates "nebulous" absorption lines due to rapid rotation. It is about 400[7] million years old with a high projected rotational velocity of 243 km/s.[3] This rate of spin is giving the star an oblate shape with a pronounced equatorial bulge that is an estimated 28% wider than the polar radius.[10]

33 Cyg has 2.33[3] times the mass of the Sun and 2.76[6] times the Sun's radius. The star is radiating 44 times the Sun's luminosity from its photosphere at an effective temperature of 8,395 K.[3] It displays an infrared excess that suggests an orbiting debris disk with a temperature of 500 K at a mean distance of 1.80 AU from the host star.[6]

References
  1. 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.
  2. 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.
  3. Zorec, J.; et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691.
  4. Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
  5. Becker, Juliette C.; et al. (April 2015), "Extracting Radial Velocities of A- and B-type Stars from Echelle Spectrograph Calibration Spectra", The Astrophysical Journal Supplement Series, 217 (2): 13, arXiv:1503.03874, Bibcode:2015ApJS..217...29B, doi:10.1088/0067-0049/217/2/29, 29.
  6. Cotten, Tara H.; Song, Inseok (July 2016), "A Comprehensive Census of Nearby Infrared Excess Stars", The Astrophysical Journal Supplement Series, 225 (1): 24, arXiv:1606.01134, Bibcode:2016ApJS..225...15C, doi:10.3847/0067-0049/225/1/15, 15.
  7. De Rosa, R. J.; et al. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216, arXiv:1311.7141, Bibcode:2014MNRAS.437.1216D, doi:10.1093/mnras/stt1932.
  8. "33 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-14.
  9. Eggen, Olin J. (December 1995), "Reality Tests of Superclusters in the Young Disk Population", Astronomical Journal, 110: 2862, Bibcode:1995AJ....110.2862E, doi:10.1086/117734.
  10. van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2.
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