Astronomy:59 Cygni
 A visual band light curve of V832 Cygni. The main plot shows the long-term variability, and the inset plot shows the variation over a single orbital period. Adapted from Harmanec et al. (2002)[1] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 20h 59m 49.55164s[2] |
| Declination | +47° 31′ 15.3789″[2] |
| Apparent magnitude (V) | 4.74[3] |
| Characteristics | |
| Spectral type | B1.5Vnne[4] + sdO + A3V + A8III + ?[5] |
| B−V color index | −0.084±0.004[3] |
| Variable type | γ Cas[6] |
| Astrometry | |
| Radial velocity (Rv) | 1.4±4.2[3] km/s |
| Proper motion (μ) | RA: +9.534[2] mas/yr Dec.: +3.090[2] mas/yr |
| Parallax (π) | 2.5088 ± 0.3226[2] mas |
| Distance | approx. 1,300 ly (approx. 400 pc) |
| Absolute magnitude (MV) | −3.37[3] |
| Orbit[7] | |
| Period (P) | 28.1871±0.0011 d |
| Eccentricity (e) | 0.141±0.008 |
| Periastron epoch (T) | 45677.6±0.3 HJD |
| Argument of periastron (ω) (secondary) | 257±4° |
| Semi-amplitude (K1) (primary) | 11.7±0.9 km/s |
| Semi-amplitude (K2) (secondary) | 121.3±1.1 km/s |
| Details[7] | |
| 59 Cyg Aa – Be star | |
| Mass | 6.3–9.4 M☉ |
| Radius | 5.5–7.0 R☉ |
| Luminosity | 7,943 L☉ |
| Surface gravity (log g) | 3.78±0.09 cgs |
| Temperature | 21,800±700 K |
| Rotational velocity (v sin i) | 379±27 km/s |
| 59 Cyg Aa – sdO | |
| Mass | 0.62–0.91 M☉ |
| Radius | 0.34–0.43 R☉ |
| Luminosity | 1,000 L☉ |
| Surface gravity (log g) | 5.0±1.0 cgs |
| Temperature | 52,100±4,800 K |
| Rotational velocity (v sin i) | < 40 km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
59 Cygni is a multiple[7] star system in the northern constellation of Cygnus, located roughly 1,300 light years away from Earth. It is visible to the naked eye as a blue-white hued star with a combined apparent visual magnitude of 4.74.[3]
The primary component and brightest member of this system, designated 59 Cyg Aa, is a rapidly rotating Be star with a stellar classification of B1.5 Vnne.[4] This is a well-studied star thanks to pronounced spectral variations that have been observed since 1916, and two short-term shell star phases that were observed in 1973 and 1974–5.[9] It is actually a confirmed spectroscopic binary system with a high temperature subdwarf O-type companion in a 28-day orbital period. The latter is heating the nearest side of the circumstellar gaseous disk that surrounds the primary.[7]
Orbiting the primary pair is 59 Cyg Ab, a magnitude 7.64 A-type main-sequence star of class A3V, located at an angular separation of 0.200″. A fourth component is a magnitude 9.8 A-type giant star of class A8III at a separation of 20.2″ along a position angle (PA) of 352°, as of 2008. The fifth companion is magnitude 11.7 at a separation of 26.7″ and a PA of 141°.[5] Gaia Data Release 2 suggests that the companions at 20.2″ and 26.7″ are respectively 382 pc and 366 pc away and moving in approximately the same direction as the primary triple.[10][11]
References
- ↑ Harmanec, P.; Božić, H.; Percy, J. R.; Yang, S.; Ruždjak, D.; Sudar, D.; Wolf, M.; Iliev, L. et al. (May 2002). "Properties and nature of Be stars". Astronomy & Astrophysics 387 (2): 580–594. doi:10.1051/0004-6361:20020453. Bibcode: 2002A&A...387..580H.
- ↑ 2.0 2.1 2.2 2.3 2.4 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.
- ↑ 3.0 3.1 3.2 3.3 3.4 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 4.0 4.1 Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement 17: 371, doi:10.1086/190179, Bibcode: 1968ApJS...17..371L.
- ↑ 5.0 5.1 Eggleton, P. P.; Tokovinin, A. A. (2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Samus, N. N. et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, GCVS 5.1 61 (1): 80–88, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S.
- ↑ 7.0 7.1 7.2 7.3 Peters, Geraldine J. et al. (March 2013), "Far-ultraviolet Detection of the Suspected Subdwarf Companion to the Be Star 59 Cygni", The Astrophysical Journal 765 (1): 8, doi:10.1088/0004-637X/765/1/2, 2, Bibcode: 2013ApJ...765....2P.
- ↑ "59 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=59+Cyg.
- ↑ Harmanec, P. et al. (May 2002), "Properties and nature of Be stars. XXI. The long-term and the orbital variations of V832 Cyg = 59 Cyg", Astronomy and Astrophysics 387 (2): 580–594, doi:10.1051/0004-6361:20020453, Bibcode: 2002A&A...387..580H.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
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