2 Cygni

In today's world, 2 Cygni has become a topic of great relevance and interest to a wide range of people. Whether it's its impact on society, its influence on popular culture, its relevance in history, or its potential for the future, 2 Cygni has captured the attention of individuals from all walks of life. From academics to entertainment lovers to professionals from various fields, everyone seems to find some value in further exploring and understanding the phenomenon of 2 Cygni. In this article, we will delve into different aspects and perspectives around 2 Cygni, with the aim of offering a comprehensive and enriching vision of this topic that is so relevant today.

2 Cygni
Observation data
Epoch J2000      Equinox J2000
Constellation Cygnus
Right ascension 19h 24m 07.57863s[1]
Declination +29° 37′ 16.7934″[1]
Apparent magnitude (V) 4.976[2]
Characteristics
Spectral type B3 IV[3]
B−V color index −0.117[2]
Astrometry
Radial velocity (Rv)−23.60±2.0[4] km/s
Proper motion (μ) RA: +12.022[1] mas/yr
Dec.: +12.173[1] mas/yr
Parallax (π)3.5657±0.1692 mas[1]
Distance910 ± 40 ly
(280 ± 10 pc)
Absolute magnitude (MV)−2.06[4]
Details
Mass7.0±0.1[5] M☉
Radius5.6[6] R☉
Luminosity (bolometric)3,354[2] L☉
Surface gravity (log g)3.653±0.035[7] cgs
Temperature16,479±219[7] K
Metallicity +0.03±0.05[8] dex
Rotational velocity (v sin i)137±8[7] km/s
Age36.6±0.5[5] Myr
Other designations
BD+29°3584, FK5 3550, GC 26785, HD 182568, HIP 95372, HR 7372, SAO 87159[9]
Database references
SIMBADdata

2 Cygni is a blue-white hued star in the northern constellation of Cygnus, located a few degrees from Albireo. It is a probable astrometric binary;[10] the visible component can be viewed with the naked eye, having an apparent visual magnitude of 4.976.[2] Based upon an annual parallax shift of 3.6 mas,[1] it is located roughly 910 light years from Earth. It has a peculiar velocity of 23 km/s and may be a runaway star[5] system.

The stellar classification of the primary is B3 IV,[3] matching a B-type subgiant star. It has seven[5] times the mass of the Sun and about 5.6[6] times the Sun's radius. The star is 37[5] million years old with a high rate of spin; it has a projected rotational velocity of 137 km/s.[7] It is radiating 3,354[2] times the Sun's luminosity from its photosphere at an effective temperature of 16,479 K.[7]

In 2024, imaging detected a candidate companion star at an angular separation of 70 mas. It appears to be a main sequence star with an estimated mass of 5.90±0.18 M☉.[11]

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 Hohle, M. M.; et al. (April 2010), "Masses and luminosities of O- and B-type stars and red supergiants", Astronomische Nachrichten, 331 (4): 349, arXiv:1003.2335, Bibcode:2010AN....331..349H, doi:10.1002/asna.200911355, S2CID 111387483.
  3. ^ a b Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode:1968ApJS...17..371L, doi:10.1086/190179.
  4. ^ a b 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.
  5. ^ a b c d e 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, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  6. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS", Astronomy and Astrophysics, 367 (2) (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  7. ^ a b c d e Huang, W.; Gies, D. R. (August 2008), "Stellar Rotation in Field and Cluster B Stars", The Astrophysical Journal, 683 (2): 1045–1051, arXiv:0805.2133, Bibcode:2008ApJ...683.1045H, doi:10.1086/590106, S2CID 18926523.
  8. ^ Gáspár, András; et al. (2016), "The Correlation between Metallicity and Debris Disk Mass", The Astrophysical Journal, 826 (2): 171, arXiv:1604.07403, Bibcode:2016ApJ...826..171G, doi:10.3847/0004-637x/826/2/171, S2CID 119241004.
  9. ^ "2 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-07.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  11. ^ Crepp, Justin R.; et al. (December 2024), Resolving the Young 2 Cygni Run-away Star into a Binary using iLocater, arXiv:2412.06982, Bibcode:2024arXiv241206982C, doi:10.48550/arXiv.2412.06982.