Psi Cygni

In the following article we will analyze in detail the importance of Psi Cygni in the current context. Psi Cygni has become a topic of great relevance in modern society, generating debates, conflicting opinions and endless repercussions in different areas. Throughout history, Psi Cygni has proven to be a determining factor in the evolution of humanity, influencing cultural, social, political and economic aspects. In this sense, it is crucial to understand the importance of Psi Cygni and its impact on the contemporary world. Through a critical and analytical approach, we will explore the various dimensions of Psi Cygni and its relevance in the current context, with the aim of providing a comprehensive vision on this topic of general interest.
Psi Cygni
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cygnus
Right ascension 19h 55m 37.78622s[1]
Declination +52° 26′ 20.2116″[1]
Apparent magnitude (V) 4.92[2] (5.05 + 7.61)[3]
Characteristics
A
Spectral type A4 Vn[4]
U−B color index +0.05[2]
B−V color index +0.13[2]
B
Spectral type F4 V[5]
Astrometry
Radial velocity (Rv)−10[6] km/s
Proper motion (μ) RA: −37.62[1] mas/yr
Dec.: −31.13[1] mas/yr
Parallax (π)11.59 ± 0.38 mas[1]
Distance281 ± 9 ly
(86 ± 3 pc)
Absolute magnitude (MV)+0.23[7]
Orbit[8]
PrimaryAa
CompanionAb
Period (P)54.08 yr
Semi-major axis (a)0.141″
Eccentricity (e)0.484
Inclination (i)112.0°
Details
ψ Cyg Aa
Luminosity62[9] L☉
Temperature7,971[9] K
Rotational velocity (v sin i)207[4] km/s
ψ Cyg B
Rotational velocity (v sin i)120[10] km/s
Other designations
ψ Cyg, 24 Cygni, BD+52° 2572, HD 189037, HIP 98055, HR 7619, SAO 32114, WDS 19556+5226.[11]
Database references
SIMBADdata

ψ Cygni, Latinised as Psi Cygni, is a triple star[3] system in the constellation called Cygnus. With a combined apparent visual magnitude of 4.92,[2] it is visible to the naked eye. As of 2002, the inner pair, components Aa and Ab, had an angular separation of 0.10 arc seconds along a position angle of 77.6°.[12] Their combined visual magnitude is 5.05.[3] Relative to this pair, the third member of the system, magnitude 7.61[3] component B, had an angular separation of 2.87 arc seconds along a position angle of 175.6° as of 2010.[13] Based upon an annual parallax shift of 11.59 mas,[1] Psi Cygni is located around 281 light years from the Sun.

The brighter member of the system, presumably component Aa, displays the spectrum of an A-type main sequence star with a stellar classification of A4 Vn,[4] where the 'n' notation indicates "nebulous" absorption lines due to rapid rotation. It appears to be a spinning with a projected rotational velocity of 207.[4] The component is radiating 62 times the solar luminosity from its outer atmosphere at an effective temperature of 7,971 K.[9]

References

  1. ^ a b c d e f 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, S2CID 18759600.
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, Bibcode:1986EgUBV........0M.
  3. ^ a b c d 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.
  4. ^ a b c d Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  5. ^ Edwards, T. W. (April 1976), "MK classification for visual binary components", Astronomical Journal, 81: 245–249, Bibcode:1976AJ.....81..245E, doi:10.1086/111879.
  6. ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. Determination of Radial Velocities and Their Applications. Vol. 30. p. 57. Bibcode:1967IAUS...30...57E.
  7. ^ 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.
  8. ^ Tokovinin, Andrei (2018). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5. S2CID 119047709.
  9. ^ a b c McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  10. ^ Uesugi, Akira; Fukuda, Ichiro (1970). Catalogue of rotational velocities of the stars. Contributions from the Institute of Astrophysics and Kwasan Observatory. Bibcode:1970crvs.book.....U.
  11. ^ "* psi Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-02-21.
  12. ^ Roberts, Lewis C. Jr. (May 2011), "Astrometric and photometric measurements of binary stars with adaptive optics: observations from 2002", Monthly Notices of the Royal Astronomical Society, 413 (2): 1200–1205, arXiv:1012.3383, Bibcode:2011MNRAS.413.1200R, doi:10.1111/j.1365-2966.2011.18205.x, S2CID 118398949.
  13. ^ Mason, Brian D.; et al. (August 2011), "Speckle Interferometry at the U.S. Naval Observatory. XVII.", The Astronomical Journal, 142 (2): 4, Bibcode:2011AJ....142...46M, doi:10.1088/0004-6256/142/2/46, S2CID 250806722, 46.
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