Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cygnus |
Right ascension | 20h 52m 3.57718s [2] |
Declination | +34° 39′ 27.4861″ [2] |
Apparent magnitude (V) | 7.3 - 7.9 [3] |
Characteristics | |
Primary | |
Spectral type | O9.5V [4] |
Apparent magnitude (U) | 5.91[ citation needed] |
Apparent magnitude (B) | 6.996[ citation needed] |
Apparent magnitude (V) | 7.287 [4] |
U−B color index | −1.086 [4] |
B−V color index | −0.291 [4] |
Secondary | |
Spectral type | O9.5V [4] |
Apparent magnitude (U) | 5.883[ citation needed] |
Apparent magnitude (B) | 6.974[ citation needed] |
Apparent magnitude (V) | 7.265 [4] |
U−B color index | −1.091 [4] |
B−V color index | −0.291 [4] |
Variable type | Algol [3] |
Astrometry | |
Proper motion (μ) |
RA: +2.763
[2]
mas/
yr Dec.: −15.981 [2] mas/ yr |
Parallax (π) | 0.6759 ± 0.0338 mas [2] |
Distance | 4,900
ly (1,500 [4] pc) |
Absolute magnitude (MV) | −3.59/−3.62 [4] |
Absolute bolometric magnitude (Mbol) | −6.65±0.04/−6.7±0.04 [4] |
Orbit [4] | |
Primary | Y Cyg A |
Companion | Y Cyg B |
Period (P) | 2.99633210±0.00000031 d |
Semi-major axis (a) | 28.72 R☉ |
Eccentricity (e) | 0.14508 |
Inclination (i) | 86.474±0.019° |
Periastron epoch (T) | 2,446,308.66407±0.0001 |
Argument of periastron (ω) (secondary) | 312.514° |
Argument of periastron (ω) (primary) | 132.514±0.052° |
Details [4] | |
Primary | |
Mass | 17.72±0.35 M☉ |
Radius | 5.785±0.091 R☉ |
Luminosity | 36,000 L☉ |
Surface gravity (log g) | 4.161±0.014 cgs |
Temperature | 33,200±200 K |
Rotational velocity (v sin i) | 132 km/s |
Age | 2 Myr |
Secondary | |
Mass | 17.73±0.3 M☉ |
Radius | 5.816±0.063 R☉ |
Luminosity | 37,700 L☉ |
Surface gravity (log g) | 4.157±0.01 cgs |
Temperature | 33,521±40 K |
Rotational velocity (v sin i) | 132 km/s |
Age | 2 Myr |
Other designations | |
Database references | |
SIMBAD | data |
Y Cygni is an eclipsing and double-lined spectroscopic binary star system in the constellation of Cygnus. It is located about 4,900 light-years from Earth. The system was one of the first binaries with a convincing detection of the apsidal precession. [4]
The two stars, being O-type main-sequence stars, orbit each other with a period of nearly 3 days. [4]
The early type of Y Cyg made it a popular target for astronomers in the past, and spectroscopic orbits have been historically computed numerous times. [5] The first of these studies was published in 1920 by John Stanley Plaskett. [6] Extensive spectroscopic studies of Y Cyg were carried out as early as 1930. [7] Several follow-ups to these have been published in 1959, [8] 1971, [9] [10] and 1980. [11] The latter of these contained an estimate of the period of apsidal precession.