23 Cygni

23 Cygni's theme is one that has captured the attention of millions of people around the world. For decades, 23 Cygni has been the subject of debate, discussion and analysis in different sectors of society. Its influence has been felt in politics, the economy, culture and daily life. In this article, we will explore various facets of 23 Cygni, from its origin and evolution to its impact today. Through a multidisciplinary approach, we will delve into the different perspectives that exist on 23 Cygni and how these have shaped our understanding and perception of this phenomenon.
23 Cygni
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 53m 17.37873s[1]
Declination +57° 31′ 24.4810″[1]
Apparent magnitude (V) 5.14[2]
Characteristics
Spectral type B5 V[3]
U−B color index +0.76[2]
B−V color index −0.13[2]
Astrometry
Radial velocity (Rv)−31.6±1.6[4] km/s
Proper motion (μ) RA: +5.768[1] mas/yr
Dec.: +11.483[1] mas/yr
Parallax (π)5.9155 ± 0.1728 mas[1]
Distance550 ± 20 ly
(169 ± 5 pc)
Absolute magnitude (MV)−1.30[5]
Details[2]
Mass4.7+0.64
−0.53[6] M☉
Radius4.30±0.45 R☉
Luminosity611.53[5] L☉
Surface gravity (log g)3.82±0.08 cgs
Temperature14,893±214 K
Metallicity −0.17±0.16 dex
Rotational velocity (v sin i)145 km/s
Age26+32
−19[6] Myr
Other designations
23 Cyg, BD+57°2084, HD 188665, HIP 97870, HR 7608, SAO 32085, WDS J19533+5731[7]
Database references
SIMBADdata

23 Cygni is a single,[2] blue-white hued star in the northern constellation Cygnus. It is a faint star, visible to the naked eye, with an apparent visual magnitude of 5.14.[2] The distance to this star, as estimated from its annual parallax shift of 5.9 mas,[1] is about 550 light years. It is moving closer to the Earth with a heliocentric radial velocity of −32 km/s,[4] and is expected to come as near as 166 light-years in around 5.6 million years.[2] At that distance, the current star would be of magnitude 2.24.[8]

This is an ordinary B-type main-sequence star of spectral type B5V, a star that is generating energy through hydrogen fusion at its core. It is roughly 26[2] million years old with 4.7[6] times the mass of the Sun and 4.3 times the Sun's radius.[2] The star has a high rate of spin, having a projected rotational velocity of 145 km/s.[2] It is radiating 612[5] times the Sun's luminosity from its photosphere at an effective temperature of 14,893 K.[2]

References

  1. ^ a b c d e f 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.
  2. ^ a b c d e f g h i j k Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal, 129 (3): 1642–1662, arXiv:astro-ph/0412542, Bibcode:2005AJ....129.1642F, doi:10.1086/427855, S2CID 119512018.
  3. ^ Hill, P. W.; Lynas-Gray, A. E. (September 1977), "UBV photometry and MK spectral classification of northern early-type stars at intermediate galactic latitudes.", Monthly Notices of the Royal Astronomical Society, 180 (4): 691–702, Bibcode:1977MNRAS.180..691H, doi:10.1093/mnras/180.4.691.
  4. ^ a b Gontcharov, G. A. (2006), "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system", Astronomy Letters, 32 (11): 759–771, arXiv:1606.08053, Bibcode:2006AstL...32..759G, doi:10.1134/S1063773706110065, S2CID 119231169.
  5. ^ a b c 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.
  6. ^ a b c Gullikson, Kevin; et al. (August 2016), "The Close Companion Mass-ratio Distribution of Intermediate-mass Stars", The Astronomical Journal, 152 (2): 13, arXiv:1604.06456, Bibcode:2016AJ....152...40G, doi:10.3847/0004-6256/152/2/40, S2CID 119179065, 40.
  7. ^ "23 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-09.
  8. ^ At a distance (D) of 50.99 and an absolute magnitude (M) of −1.30, ignoring extinction (A), the apparent magnitude (m) would be:
    m = M + A + 5·log D + 5 ≈ −1.30 + 5·log 50.99 − 5 = 2.24
    Ref.: Dopita, Michael A.; Sutherland, Ralph S. (2004), Astrophysics of the Diffuse Universe, Astronomy and Astrophysics Library, Springer Science & Business Media, p. 296, ISBN 3540433627
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