V1057 Cygni
File:V1057CygLightCurve.png 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 Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Cygnus |
| Right ascension | Template:RA[3] |
| Declination | Template:DEC[3] |
| Apparent magnitude (V) | Script error: No such module "val".[4] |
| Characteristics | |
| Spectral type | F7/G3 I/IIe[5] |
| B−V Template:Engvar | 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 mas[3] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Details | |
| Radius | Script error: No such module "val".[3] Template:Solar radius |
| Luminosity | Script error: No such module "val".[3] Template:Solar luminosity |
| Temperature | Script error: No such module "val".[3] K |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist, LkHα 190, AAVSO 2055+43[7] | |
| Database references | |
| SIMBAD | data |
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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–Script error: No such module "val"..[4]
A faint binary companion was discovered in 2016, and designated component B. It is located at a projected separation of Script error: No such module "val". 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
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