Observation data Equinox J2000.0]] (ICRS) | |
---|---|
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[2] mas |
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 periapsis (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 | |
Y Cyg, HD 198846, HIP 102999 | |
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.
Original source: https://en.wikipedia.org/wiki/Y Cygni.
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