V404 Cygni

V404 Cygni

X-ray light echoes from the 2015 nova eruption
Credit: Andrew Beardmore (Univ. of Leicester) and NASA/Swift
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Cygnus
Right ascension 20h 24m 03.82s
Declination +33° 52 02.0
Apparent magnitude (V) 11.2 - 18.8
Characteristics
Spectral type K3 III
U−B color index +0.3
B−V color index +1.5
Variable type Nova
Astrometry
Proper motion (μ) RA: −5.177 mas/yr
Dec.: −7.778 mas/yr
Parallax (π)0.3024±0.0783 mas
Distance2,390 pc
Absolute magnitude (MV)+3.4
Details
A (black hole)
Mass9 M
B
Mass0.7 M
Radius6.0 R
Luminosity10.2 L
Surface gravity (log g)3.50 cgs
Temperature4,800 K
Metallicity [Fe/H]+0.23 dex
Rotational velocity (v sin i)36.4 km/s
C
Mass1.2 M
Radius1.85 R
Surface gravity (log g)3.95 cgs
Temperature6123 K
Metallicity [Fe/H]-0.09 dex
Age4 Gyr
Other designations
V404 Cyg, Nova Cygni 1938, Nova Cygni 1989, GS 2023+338, AAVSO 2020+33
Database references
SIMBADdata

V404 Cygni is a microquasar and a triple star system in the constellation of Cygnus. It contains a black hole with a mass of about 9 M and an early K giant star companion with a mass slightly smaller than the Sun, and an evolved tertiary component. The inner star and the black hole orbit each other every 6.47129 days at fairly close range, while the outer tertiary takes 70000 years to orbit the inner binary system. Due to their proximity and the intense gravity of the black hole, the secondary star loses mass to an accretion disk around the black hole and ultimately to the black hole itself.

The "V" in the name indicates that it is a variable star, which repeatedly gets brighter and fainter over time. It is also considered a nova, because at least three times in the 20th century it produced a bright outburst of energy. Finally, it is a soft X-ray transient because it periodically emits short bursts of X-rays.

The black hole companion has been proposed as a Q star candidate.