Astronomy:V1057 Cygni
 A visual band light curve for V1057 Cygni. The main plot shows the long-term variability, and the inset shows the short-term variability. Adapted from Kopatskaya et al. (2002)[1] and Clarke et al. (2005).[2] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 20h 58m 53.73367s[3] |
| Declination | +44° 15′ 28.3847″[3] |
| Apparent magnitude (V) | 12.43±0.03[4] |
| Characteristics | |
| Spectral type | F7/G3 I/IIe[5] |
| B−V color index | 1.93[6] |
| Variable type | FU Ori |
| Astrometry | |
| Proper motion (μ) | RA: −2.793[3] mas/yr Dec.: −3.813[3] mas/yr |
| Parallax (π) | 1.0864 ± 0.0388[3] mas |
| Distance | 3,000 ± 100 ly (920 ± 30 pc) |
| Details | |
| Radius | 16.2+1.2 −3.2[3] R☉ |
| Luminosity | 38.3±2.0[3] L☉ |
| Temperature | 3,565+414 −127[3] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
V1057 Cygni is a suspected binary star[8] system in the northern constellation of Cygnus. It is a variable star of the FU Orionis-type, and was the second FU Orionis-type variable to be discovered. The system is located at a distance of approximately 3,000 light years from the Sun,[3] in the North America Nebula.[4] It has an apparent visual magnitude of around 12.4.[4]
The initial classification of the primary was as a young T Tauri star.[4] During 1969–1970 it underwent a nova-like outburst, increasing in brightness by five magnitudes and emitting a strong mass outflow. For the next ten years the brightness stayed at a plateau before decreasing rapidly in the mid–1990s, accompanied by a change in its spectrum. As of 2013, it is 1.5 magnitudes brighter than it was before the nova-like event.[8] The mass of FU Ori objects is estimated to be in the range of 0.3–0.7 M☉.[4]
A faint binary companion was discovered in 2016, and designated component B. It is located at a projected separation of 30±5 astronomical unit|AU from the primary, with a possible orbital period of ~300 years. The 1970 outburst of the primary may have been caused by torque of its accretion disk by the companion.[4]
References
- ↑ Kopatskaya, E. N.; Grinin, V. P.; Shakhovskoi, D. N.; Shulov, O. S. (April 2002). "Results of Photometric and Polarimetric Observations of the Fuor V1057 Cyg from the Time of an Outburst to the Present". Astrophysics 45 (2): 143–149. doi:10.1023/A:1016052529802. Bibcode: 2002Ap.....45..143K. https://ui.adsabs.harvard.edu/abs/2002Ap.....45..143K. Retrieved 21 December 2021.
- ↑ Clarke, C.; Lodato, G.; Melnikov, S. Y.; Ibrahimov, M. A. (August 2005). "The photometric evolution of FU Orionis objects: disc instability and wind–envelope interaction". Monthly Notices of the Royal Astronomical Society 361 (3): 942–954. doi:10.1111/j.1365-2966.2005.09231.x. Bibcode: 2005MNRAS.361..942C.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 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.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Green, Joel D. et al. (October 2016). "Testing the Binary Trigger Hypothesis in FUors". The Astrophysical Journal 830 (1): 5. doi:10.3847/0004-637X/830/1/29. 29. Bibcode: 2016ApJ...830...29G.
- ↑ Herbig, G. H. et al. (2003). "High-Resolution Spectroscopy of FU Orionis Stars". The Astrophysical Journal 595 (1): 384–411. doi:10.1086/377194. Bibcode: 2003ApJ...595..384H.
- ↑ Zacharias, N. (2012). "The fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". VizieR On-line Data Catalog 1322 (2): 44. doi:10.1088/0004-6256/145/2/44. Bibcode: 2012yCat.1322....0Z.
- ↑ "LkHA 190". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=LkHA+190.
- ↑ 8.0 8.1 Kopatskaya, E. N. et al. (September 2013). "Photometric behaviour of the FU Orionis type star, V1057 Cygni, during the last 25 years". Monthly Notices of the Royal Astronomical Society 434 (1): 38–45. doi:10.1093/mnras/stt963. Bibcode: 2013MNRAS.434...38K.
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