39 Cygni

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39 Cygni
Observation data
Epoch J2000       Equinox J2000
Constellation Cygnus
Right ascension 20h 23m 51.6138s [1]
Declination +32° 11′ 24.4816″ [1]
Apparent magnitude  (V)4.43 [2]
Characteristics
Evolutionary stage Giant star
Spectral type K2.5 III Fe−0.5 [3]
U−B color index 1.50 [4]
B−V color index 1.331±0.003 [2]
Astrometry
Radial velocity (Rv)−14.47±0.45 [1]  km/s
Proper motion (μ)RA: +52.762  mas/yr [1]
Dec.: +0.309  mas/yr [1]
Parallax (π)12.2359 ± 0.1273  mas [1]
Distance 267 ± 3  ly
(81.7 ± 0.9  pc)
Absolute magnitude  (MV)0.01 [2]
Orbit [4]
Period (P)85.67 ± 0.89 yr
Eccentricity (e)0.495±0.023
Periastron epoch (T)2,453,794±174  JD
Argument of periastron (ω)
(secondary)		177±7°
Semi-amplitude (K1)
(primary)		3.23±0.11 km/s
Details
39 Cyg A
Mass 1.9±0.1 [5]   M☉
Radius 25±1 [5]   R☉
Luminosity 186+14
−12 [6]   L☉
Surface gravity (log g)1.83±0.03 [5]   cgs
Temperature 4,284±125 [5]   K
Metallicity [Fe/H]0.04 [5]   dex
Rotational velocity (v sin i)5.6 [7]  km/s
Age 3.86±1.89 [6]   Gyr
Other designations
39 Cyg, BD+31°4062, FK5  3633, GC  28378, HD  194317, HIP  100587, HR  7806, SAO  69950, GSC  02676-01688 [8]
Database references
SIMBAD data

39 Cygni is a binary star [9] system near the southern border [4] of the northern constellation of Cygnus, approximately 270 light years away from Earth. [1] It is visible to the naked eye as an orange-hued star with an apparent visual magnitude of 4.43. [2] The system is moving closer to the Sun with a heliocentric radial velocity of −15 km/s. [1]

This is a single-lined spectroscopic binary with an orbital period of about 85.67 years (31,292 d) and an eccentricity of 0.5. The projected semi-major axis of the primary star's orbit is 1,207 ± 46 Gm (8.07 ± 0.31  AU ), providing a lower bound on the separation of the stars. [4] The system is around four billion years old. [6]

The visible component is an evolved K-type giant star with a stellar classification of K2.5 III Fe−0.5; [3] the suffix notation indicates a mild underabundance of iron in the spectrum. It is probably on the horizontal branch, fusing helium in its core, but may be on the red giant branch fusing hydrogen in a shell around an insert helium core. [10] It has 1.9 times the mass of the Sun and has expanded to 25 times the Sun's radius. The star is radiating 186 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,284 K. [5]

The unseen secondary component is most probably a main sequence star with a type between F and mid-K, although it may be a white dwarf instead. Its mass is at least 0.7–1.0 times the mass of the Sun. [4]

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3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

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<span class="mw-page-title-main">30 Vulpeculae</span> Star in the constellation Vulpecula

30 Vulpeculae is a binary star system in the northern constellation of Vulpecula, located mid-way between Epsilon Cygni and a diamond-shaped asterism in Delphinus. It is visible to the naked eye as a faint, orange-hued point of light with an apparent visual magnitude of 4.91. The system is located approximately 350 light years away from the Sun based on parallax, and is drifting further away with a mean radial velocity of +30 km/s. The system has a relatively high proper motion, traversing the celestial sphere at the rate of 0.186 arc seconds per annum.

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<span class="mw-page-title-main">Eta Cygni</span> Star in the constellation Cygnus

Eta Cygni is a star in the northern constellation of Cygnus. It is visible to the naked eye with an apparent visual magnitude of 3.889. The star lies along the main body of the constellation, about midway between Gamma Cygni and Albireo. Based upon an annual parallax shift of 23.55 mas, it is located 138.5 light years from the Sun.

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6 Persei is a binary star system in the northern constellation of Andromeda. It is faintly visible to the naked eye with an apparent visual magnitude of 5.29. The system is located 182 light years from Earth, as determined from its annual parallax shift of 17.9 mas. It is moving further away with a heliocentric radial velocity of +42 km/s. The system has a relatively high rate of proper motion, traversing the celestial sphere at the rate of 0.386 arcsecond/year.

<span class="mw-page-title-main">Phi Cygni</span> Star in the constellation Cygnus

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μ Cygni, Latinised as Mu Cygni, is a binary star system in the northern constellation of Cygnus. It is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.49. The system is located 72 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of +17 km/s.

Phi3 Hydrae is a binary star in the equatorial constellation of Hydra. It originally received the Flamsteed designation of 2 Crateris before being placed in the Hydra constellation. Based upon an annual parallax shift of 15.49 mas as seen from Earth, it is located around 211 light years from the Sun. It is visible to the naked eye with an apparent visual magnitude of 4.90. It forms a triangle with the fainter φ1 Hydrae and φ2 Hydrae, between μ Hydrae and ν Hydrae.

HD 3322 is a binary star system in the northern constellation of Andromeda. With an apparent visual magnitude of 6.51, it lies below the nominal brightness limit for visibility with the normal naked eye, but it is still possible to see the star with excellent vision under ideal seeing conditions. An annual parallax shift of 4.59±0.65 mas provides a distance estimate of roughly 700 light years.

4 Cygni is a binary star system in the northern constellation of Cygnus. It is a faintly visible to the naked eye with an apparent visual magnitude of 5.17. The distance to 4 Cygni, as determined from its annual parallax shift of 5.8 mas, is about 560 light years.

References

  1. 1 2 3 4 5 6 7 8 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 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.
  3. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  4. 1 2 3 4 5 Griffin, R. F. (June 2008), "Spectroscopic binary orbits from photoelectric radial velocities - Paper 200: Kappa Persei, Beta Leonis Minoris, 56 Ursae Majoris, HR 4593, and 39 Cygni", The Observatory, 128: 176–231, Bibcode:2008Obs...128..176G.
  5. 1 2 3 4 5 6 Kallinger, T.; Beck, P. G.; Hekker, S.; Huber, D.; Kuschnig, R.; Rockenbauer, M.; Winter, P. M.; Weiss, W. W.; Handler, G.; Moffat, A. F. J.; Pigulski, A.; Popowicz, A.; Wade, G. A.; Zwintz, K. (2019-04-01), "Stellar masses from granulation and oscillations of 23 bright red giants observed by BRITE-Constellation", Astronomy & Astrophysics, 624: A35, arXiv: 1902.07531 , Bibcode:2019A&A...624A..35K, doi: 10.1051/0004-6361/201834514 , ISSN   0004-6361.
  6. 1 2 3 Maldonado, J.; et al. (June 2013), "The metallicity signature of evolved stars with planets", Astronomy & Astrophysics, 554: 18, arXiv: 1303.3418 , Bibcode:2013A&A...554A..84M, doi:10.1051/0004-6361/201321082, S2CID   119289111, A84.
  7. ↑ Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi: 10.1088/0004-6256/135/1/209 , S2CID   121883397.
  8. ↑ "39 Cyg". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-01-14.
  9. ↑ 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.
  10. ↑ Stock, S.; Reffert, S.; Quirrenbach, A. (August 2018). "Precise radial velocities of giant stars. X. Bayesian stellar parameters and evolutionary stages for 372 giant stars from the Lick planet search". Astronomy & Astrophysics. 616: 15. arXiv: 1608.00963 . Bibcode:2018A&A...616A..33S. doi:10.1051/0004-6361/201833111. S2CID   119361866. A33.
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