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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<span class="mw-page-title-main">Omega Cassiopeiae</span> Binary star system in constellation Cassiopeia

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HD 59686 is a binary star system in the northern constellation of Gemini. It is visible to the naked eye as a dim point of light with an apparent visual magnitude of +5.45. The distance to this system is approximately 292 light years based on parallax, but it is drifting closer with a radial velocity of −34 km/s.

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

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HR 7135 is a binary star system. Despite its Flamsteed designation of 62 Serpentis, the star can be found in the equatorial constellation of Aquila, in front of a dark rift in the Milky Way near the constellation border. It is visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.57. The system is located 283 light years distant from the Sun, based on parallax, and is drifting further away with a radial velocity of 23 km/s.

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

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HD 106760 is a single-lined spectroscopic binary star system in the northern constellation of Coma Berenices. It is faintly visible to the naked eye, having an apparent visual magnitude of 4.99. The system is located around 318 light years away, as determined from its annual parallax shift of 10.2417 mas. It is moving closer with a heliocentric radial velocity of −40 km/s, and is expected to come as close as 259 ly in about 772,000 years.

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.

<span class="mw-page-title-main">33 Piscium</span> Star in the constellation Pisces

33 Piscium is a binary star system in the zodiac constellation of Pisces. It is visible to the naked eye with an apparent visual magnitude of 4.61. The distance to this system, as determined from an annual parallax shift of 25.32±0.53 mas, is about 129 light years. It is moving closer to the Sun with a heliocentric radial velocity of −6.6 km/s.

20 Cygni is a single, orange-hued star in the northern constellation of Cygnus. It is a faint star but is visible to the naked eye with an apparent visual magnitude of 5.03. The distance to 20 Cygni can be estimated from its annual parallax shift of 16 mas, which yields a range of 202 light years. It is moving closer to the Earth with a heliocentric radial velocity of −22 km/s.

26 Cygni is a single star in the northern constellation of Cygnus. It has the Bayer designation e Cygni, while 26 Cygni is the Flamsteed designation. This star is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 5.12. It is located around 451 light-years (138 pc) distant from the Sun, based on parallax measurements. The radial velocity is close to negligible, being measured at −0.3 km/s.

71 Cygni is a star in the northern constellation of Cygnus, located 212 light years from the Sun. 71 Cygni is the Flamsteed designation; it has the Bayer designation g Cygni. It is visible to the naked eye as a dim, orange-hued star with an apparent visual magnitude of 5.22. The star is moving closer to the Earth with a heliocentric radial velocity of −21.5 km/s.

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.

16 Serpentis is a binary star system in the Serpens Caput portion of the equatorial constellation of Serpens, located 228 light years from the Sun. It is visible to the naked eye as a fain, orange-hued star with an apparent visual magnitude of 5.261. The system is moving further from the Earth with a heliocentric radial velocity of +3 km/s.

HD 193373 is a solitary red hued star located in the equatorial constellation Delphinus. It has an apparent magnitude of 6.21, placing it near the limit for naked eye visibility. Parallax measurements place it 846 light years distant and it is currently receding with a heliocentric radial velocity of 22.7 km/s.

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 , 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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