R Cygni
R Cygni's theme is one that has captivated the attention of many people over time. Whether due to its relevance in history, its impact on current society, or its importance in the academic field, R Cygni has been the object of study, debate and reflection. In this article, we will explore different aspects related to R Cygni, from its origin and evolution, to its influence in various areas. Through a deep and detailed analysis, we will seek to better understand the importance and role that R Cygni plays in today's world. Without a doubt, R Cygni is a topic that continues to generate interest and curiosity in many people, and we hope to be able to offer a complete and enriching overview of this fascinating topic.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 19h 36m 49.35633s[1] |
| Declination | +50° 11′ 59.7198″[1] |
| Apparent magnitude (V) | 6.1 - 14.4[2] |
| Characteristics | |
| Spectral type | S2.5,9e-S6,9e(Tc)[3] |
| Variable type | Mira[2] |
| Astrometry | |
| Proper motion (μ) | RA: −3.158[1] mas/yr Dec.: −5.755[1] mas/yr |
| Parallax (π) | 1.4835±0.0963 mas[1] |
| Distance | 2,200 ± 100 ly (670 ± 40 pc) |
| Details | |
| Mass | 0.85[4] M☉ |
| Luminosity | 11,700[5] L☉ |
| Surface gravity (log g) | −0.50[4] cgs |
| Temperature | 2,538[4] K |
| Metallicity | +0.50[4] dex |
| Other designations | |
| R Cyg, AAVSO 1934+49, BD+49 3064, HD 185456, HIP 31822, SAO 31822, WDS J19368+5012[6] | |
| Database references | |
| SIMBAD | data |
R Cygni is a variable star of the Mira type in the constellation Cygnus, less than 4' from θ Cygni. This is a red giant star on the asymptotic giant branch located around 2,200 light years away. It is an S-type star ranging between spectral types S2.5,9e to S6,9e(Tc).[3]
Stars at this mass range and evolutionary stage are pulsationally unstable, displaying a variation in their light output.[7] R Cygni has a maximum magnitude of 6.1 and a minimum magnitude of 14.4, with a period of 426.45 days.[2] The variation of this star was discovered by English astronomer N. R. Pogson in 1852, and it has a history of recorded brightness measurements stretching back more than a century.[7] R Cygni shows distinct period-doubling, where alternate maxima are of different brightness, hence the real period of pulsation could be considered to be twice that from one maximum to the next.[7]
The Catalog of Components of Double and Multiple Stars lists 10th magnitude BD+49 3065 as a companion to R Cygni, at a separation of 91", and both stars lie at approximately the same distance. The Washington Double Star Catalog additionally lists a 15th magnitude star as a companion at a separation of about 14".[8]
See also
References
- ^ 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 Samus', N. N; Kazarovets, E. V; Durlevich, O. V; Kireeva, N. N; Pastukhova, E. N (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports. 61 (1): 80. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869.
- ^ a b BSJ (4 January 2010). "R Cygni". AAVSO Website. American Association of Variable Star Observers. Retrieved 21 January 2014.
- ^ a b c d Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardevol, J.; Casamiquela, L.; Figueras, F.; Jimenez-Arranz, O.; Jordi, C.; Monguio, M.; Romero-Gomez, M.; Altamirano, D.; Antoja, T.; Assaad, R.; Cantat-Gaudin, T.; Castro-Ginard, A.; Enke, H.; Girardi, L.; Guiglion, G.; Khan, S.; Luri, X.; Miglio, A.; Minchev, I.; Ramos, P.; Santiago, B. X.; Steinmetz, M. (2022). "VizieR Online Data Catalog: StarHorse2, Gaia EDR3 photo-astrometric distances (Anders+, 2022)". Vizier Online Data Catalog. Bibcode:2022yCat.1354....0A.
- ^ Guandalini, R; Francis, Charles (2010). "Infrared photometry and evolution of mass-losing AGB stars. III. Mass loss rates of MS and S stars". Astronomy and Astrophysics. 513: A4. arXiv:1002.2458. Bibcode:2010A&A...513A...4G. doi:10.1051/0004-6361/200911764. S2CID 119193286.
- ^ "R Cyg". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 30 August 2018.
- ^ a b c Kiss, L. L.; Szatmáry, K. (August 2002). "Period-doubling events in the light curve of R Cygni: Evidence for chaotic behaviour". Astronomy and Astrophysics. 390 (2): 585–596. arXiv:astro-ph/0205334. Bibcode:2002A&A...390..585K. doi:10.1051/0004-6361:20020744. S2CID 17698877.
- ^ Mason, Brian D; Wycoff, Gary L; Hartkopf, William I; Douglass, Geoffrey G; Worley, Charles E (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.