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 | 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 mas[3] |
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 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]