 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) and Clarke et al. (2005). | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | 20 58 53.73367 |
| Declination | +44° 15′ 28.3847″ |
| Apparent magnitude (V) | 12.43±0.03 |
| Characteristics | |
| Spectral type | F7/G3 I/IIe |
| B−V color index | 1.93 |
| Variable type | FU Ori |
| Astrometry | |
| Proper motion (μ) | RA: −2.793 mas/yr Dec.: −3.813 mas/yr |
| Parallax (π) | 1.0864 ± 0.0388 mas |
| Distance | 3,000 ± 100 ly (920 ± 30 pc) |
| Details | |
| Radius | 16.2+1.2 −3.2 R☉ |
| Luminosity | 38.3±2.0 L☉ |
| Temperature | 3,565+414 −127 K |
| Other designations | |
| V1057 Cyg, LkHα 190, AAVSO 2055+43 | |
| Database references | |
| SIMBAD | data |
V1057 Cygni is a suspected binary star 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, in the North America Nebula. It has an apparent visual magnitude of around 12.4.
The initial classification of the primary was as a young T Tauri star. 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. The mass of FU Ori objects is estimated to be in the range of 0.3–0.7 M☉.
A faint binary companion was discovered in 2016, and designated component B. It is located at a projected separation of 30±5 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.
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. Bibcode:2002Ap.....45..143K. doi:10.1023/A:1016052529802. S2CID 117012043. 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. arXiv:astro-ph/0505515. Bibcode:2005MNRAS.361..942C. doi:10.1111/j.1365-2966.2005.09231.x.
- ^ 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.
- ^ Green, Joel D.; et al. (October 2016). "Testing the Binary Trigger Hypothesis in FUors". The Astrophysical Journal. 830 (1): 5. arXiv:1605.03270. Bibcode:2016ApJ...830...29G. doi:10.3847/0004-637X/830/1/29. S2CID 118652194. 29.
- Herbig, G. H.; et al. (2003). "High-Resolution Spectroscopy of FU Orionis Stars". The Astrophysical Journal. 595 (1): 384–411. arXiv:astro-ph/0306559. Bibcode:2003ApJ...595..384H. doi:10.1086/377194. S2CID 119436366.
- Zacharias, N. (2012). "The fourth US Naval Observatory CCD Astrograph Catalog (UCAC4)". VizieR On-line Data Catalog. 1322 (2): 44. arXiv:1212.6182. Bibcode:2012yCat.1322....0Z. doi:10.1088/0004-6256/145/2/44. S2CID 119299381.
- "LkHA 190". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2020-11-16.
- ^ 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. Bibcode:2013MNRAS.434...38K. doi:10.1093/mnras/stt963.