Summary
74 Cygni is a visual binary[9] star system in the northern constellation Cygnus, located around 249 light years distant from the Sun. It is visible to the naked eye as a faint, white-hued star with a combined apparent visual magnitude of 5.04.[2] The pair orbit each other with a period of 1.57 years and an eccentricity of 0.5.[5] The system is a source of X-ray emission, which is most likely coming from the secondary component.[10]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 21h 36m 56.97051s[1] |
| Declination | +40° 25′ 48.5818″[1] |
| Apparent magnitude (V) | 5.04[2] |
| Characteristics | |
| Evolutionary stage | main sequence[3] |
| Spectral type | A3 Vn[4] |
| B−V color index | 0.198±0.003[2] |
| Astrometry | |
| Radial velocity (Rv) | 5.3±2.9 km/s |
| Proper motion (μ) | RA: +2.270[1] mas/yr Dec.: +18.399[1] mas/yr |
| Parallax (π) | 13.0909 ± 0.2893 mas[1] |
| Distance | 249 ± 6 ly (76 ± 2 pc) |
| Absolute magnitude (MV) | 0.95[2] |
| Orbit[5] | |
| Period (P) | 574.632±9.4158 d |
| Semi-major axis (a) | 8.56±0.91 mas |
| Eccentricity (e) | 0.5349±0.1066 |
| Inclination (i) | 102.1±4.39° |
| Longitude of the node (Ω) | 18.92° |
| Periastron epoch (T) | 8579.5387±18.6175 |
| Argument of periastron (ω) (secondary) | 306.56±14.01° |
| Details | |
| 74 Cyg A | |
| Mass | 1.68[6] M☉ |
| Radius | 1.6[7] R☉ |
| Luminosity | 35.64[2] L☉ |
| Surface gravity (log g) | 3.89[6] cgs |
| Temperature | 7,859±267[6] K |
| Rotational velocity (v sin i) | 201[3] km/s |
| Age | 606[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
The primary component is an A-type main-sequence star with a stellar classification of A3 Vn;[4] a star that is fusing its core hydrogen. The 'n' suffix indicates "nebulous" absorption lines due to rapid rotation, with the star having a projected rotational velocity of 201 km/s.[3] The high rate of spin is giving the star an oblate shape with an equatorial bulge that is 8% larger than the polar radius.[11] The star has 1.68[6] times the mass of the Sun and is radiating 36[2] times the Sun's luminosity from its photosphere at an effective temperature of about 7,859 K.[6]
References edit
- ^ a b c d e 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.
- ^ a b c d e f 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.
- ^ a b c Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
- ^ a b Abt, Helmut A.; Morrell, Nidia I. (1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
- ^ a b ESA (1997), "The HIPPARCOS and TYCHO catalogues. Astrometric and photometric star catalogues derived from the ESA HIPPARCOS Space Astrometry Mission", Esa Special Publication, 1200, Bibcode:1997ESASP1200.....E, ISBN 9290923997.
- ^ a b c d e f David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics, 367 (Third ed.): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
- ^ "74 Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-01-20.
- ^ 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Schröder, C.; Schmitt, J. H. M. M. (November 2007), "X-ray emission from A-type stars", Astronomy and Astrophysics, 475 (2): 677–684, Bibcode:2007A&A...475..677S, doi:10.1051/0004-6361:20077429.
- ^ van Belle, Gerard T. (March 2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.