Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 27m 52.40539s [2] |
Declination | +34° 46′ 58.3435″ [2] |
Apparent magnitude (V) | 8.19 to 8.83 [3] |
Characteristics | |
Spectral type | B0p + B1Vp [3] + ? |
U−B color index | -0.66 |
B−V color index | 0.18 |
Variable type | Eclipsing binary [4] |
Astrometry | |
Radial velocity (Rv) | 9 ± 5 km/s |
Proper motion (μ) |
RA: −4.479
[2]
mas/
yr Dec.: -9.049 [2] mas/ yr |
Parallax (π) | 0.4786 ± 0.5765 mas [2] |
Other designations | |
Database references | |
SIMBAD | data |
IU Aurigae is a triple star [6] system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. [7] This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19. [3] The eclipsing pair form a Beta Lyrae-type semidetached binary of two Bp stars [3] with a period of 1.81147435 days. [4] During the primary eclipse, the visual magnitude of the system drops to 8.89, while for the secondary it decreases to 8.74. [3] [8] The third component is a massive object with 17–18 M☉, and may actually be a binary – which would make this a quadruple star system. [7]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 27m 52.40539s [2] |
Declination | +34° 46′ 58.3435″ [2] |
Apparent magnitude (V) | 8.19 to 8.83 [3] |
Characteristics | |
Spectral type | B0p + B1Vp [3] + ? |
U−B color index | -0.66 |
B−V color index | 0.18 |
Variable type | Eclipsing binary [4] |
Astrometry | |
Radial velocity (Rv) | 9 ± 5 km/s |
Proper motion (μ) |
RA: −4.479
[2]
mas/
yr Dec.: -9.049 [2] mas/ yr |
Parallax (π) | 0.4786 ± 0.5765 mas [2] |
Other designations | |
Database references | |
SIMBAD | data |
IU Aurigae is a triple star [6] system in the constellation Auriga, consisting of an eclipsing binary pair orbiting a third component with a period of 335 years. [7] This system is too faint to be viewed with the naked eye, having a peak apparent visual magnitude of 8.19. [3] The eclipsing pair form a Beta Lyrae-type semidetached binary of two Bp stars [3] with a period of 1.81147435 days. [4] During the primary eclipse, the visual magnitude of the system drops to 8.89, while for the secondary it decreases to 8.74. [3] [8] The third component is a massive object with 17–18 M☉, and may actually be a binary – which would make this a quadruple star system. [7]