IU Aurigae
File:IUAurLightCurve.png A visual band light curve for IU Aurigae, adapted from Özdemir et al. (2003)[1] | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | Template:RA[2] |
| Declination | Template:DEC[2] |
| Apparent magnitude (V) | 8.19 to 8.83[3] |
| Characteristics | |
| Spectral type | B0p + B1Vp[3] + ? |
| U−B Template:Engvar | -0.66 |
| B−V Template:Engvar | 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 | |
| Template:Odlist[5] | |
| Database references | |
| SIMBAD | data |
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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]
Pavel Mayer discovered that the star's brightness varies in 1964.[8] 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][9] The third component is a massive object with 17–18 Template:Solar mass, and may actually be a binary – which would make this a quadruple star system.[7]
References
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