BC Cygni is visible as a red star (circled). The bright star at the centre is γ Cygni and north is to the right. Credit: Erik Larsen | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cygnus |
Right ascension | 20h 21m 38.55s [1] |
Declination | +37° 31′ 58.9″ [1] |
Apparent magnitude (V) | 9.0 - 10.8 [2] |
Characteristics | |
Spectral type | M3.5 Ia [3] (M2 - M5 [4] ) |
B−V color index | +3.13 - +3.21 [4] |
Variable type | SRc [3] |
Astrometry | |
Radial velocity (Rv) | −20.97 [1] km/s |
Proper motion (μ) | RA: −3.710 mas/yr [1] Dec.: −6.307 mas/yr [1] |
Parallax (π) | 0.5760±0.0500 mas [1] |
Distance | 5,418+470 −430 ly (1,662+144 −132 pc) [5] |
Absolute magnitude (MV) | −7.71 [6] |
Details | |
Mass | 19 [4] [7] M☉ |
Radius | 1,187 [1] R☉ |
Luminosity | 150,000 [7] 204,000+159,000 −56,000 [8] L☉ |
Temperature | 3,535 [7] K |
Age | >9 [7] [a] Myr |
Other designations | |
BC Cyg, HIP 100404, HV 3339, BD+37°3903, IRAS 20197+3722, 2MASS J20213855+3731589 | |
Database references | |
SIMBAD | data |
BC Cygni (BC Cyg, HIP 100404, BD + 37 3903) is a red supergiant and pulsating variable star of spectral type M3.5Ia in the constellation Cygnus.
It is considered a member of the stellar Cygnus OB1 association, and within it the open cluster Berkeley 87, [9] which would place at a distance of 1,673 parsecs (5,000 ly) of the Solar System; [10] it is less than a degree north of another variable red supergiant, BI Cygni. According to its Gaia Data Release 3 parallax, it is at about 1,700 pc. [1]
BC Cygni was found to have a luminosity of 145,000 L☉ and an effective temperature of 2,858 K in the year 1900, and a luminosity of 112,000 L☉ and a temperature of 3,614 K in the year 2000. It is one of largest stars known, at its brightest and coolest calculated to be 1,553 R☉ compared to 856 R☉ at its hottest and faintest. [11] If it were in the place of the Sun, its photosphere would engulf the entire inner Solar System and reach close to the orbit of Jupiter. With a mass of about 19 M☉, it is estimated that the stellar mass loss, as dust, as the atomic and molecular gas could not be evaluators is 3.2×10−9 M☉ per year. [12]
Louisa Wells discovered that the star's brightness varied, based on the examination of 15 photographic plates. That discovery was announced in 1911. [14] It was given its variable star designation, BC Cygni, in 1914. [15] The brightness of BC Cyg varies from visual magnitude +9.0 and +10.8 with a period of 720 ± 40 days. [2] Between around the year 1900 and 2000 appears to have increased its average brightness of 0.5 magnitudes. [4]