AE Aurigae
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Star AE Aurigae |
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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| Constellation | Carter | ||||||||||||||||
| Right ascension | 05 h 16 m 18.15 s | ||||||||||||||||
| declination | + 34 ° 18 ′ 44.3 ″ | ||||||||||||||||
| Apparent brightness | 5.96 mag 5.78 to 6.08 mag |
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| Typing | |||||||||||||||||
| B − V color index | +0.22 | ||||||||||||||||
| U − B color index | −0.70 | ||||||||||||||||
| Spectral class | O9.5 V | ||||||||||||||||
| Variable star type | Orion Variator (INA) | ||||||||||||||||
| Astrometry | |||||||||||||||||
| Radial velocity | (56.7 ± 0.6) km / s | ||||||||||||||||
| parallax | (2.46 ± 0.07) mas | ||||||||||||||||
| distance | (1325 ± 40) ly (405 ± 10) pc |
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| Visual absolute brightness M vis | −2.3 mag | ||||||||||||||||
| Proper movement | |||||||||||||||||
| Rec. Share: | (−4.44 ± 0.12) mas / a | ||||||||||||||||
| Dec. portion: | (43.37 ± 0.08) mas / a | ||||||||||||||||
| Physical Properties | |||||||||||||||||
| Dimensions | ~ 17 M ☉ | ||||||||||||||||
| radius | ~ 5 R ☉ | ||||||||||||||||
| Luminosity |
~ 30,000 L ☉ |
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| Effective temperature | ~ 36 500 K | ||||||||||||||||
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Other names and catalog entries |
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AE Aurigae ( AE Aur for short ) is a main sequence star of the spectral class O9 in the constellation Fuhrmann, about 1320 light years away from Earth . As an Orion variable , its apparent brightness fluctuates irregularly between 5.78 mag and 6.08 mag. Its intense light illuminates the emission and reflection nebula IC 405 .
Like My Columbae and 53 Arietis , AE Aurigae is one of the so-called runaway stars that move away from a star association at high space velocities . In the case of the three stars mentioned, their speeds and directions of movement suggest that they were around 3 million years ago near the present-day trapezoid in the constellation Orion, were driven out of the Orion association and flew away in different directions. According to one theory, the three stars originally formed a multiple system in Orion with a more massive fourth star, until this fourth component exploded as a supernova about 3 million years ago due to its large mass and the energy released in the process hurled the other three stars out of the Orion association. When viewed from Earth, AE Aurigae then moved at high speed from its place of origin in Orion to its current position in the constellation Fuhrmann. Another theory is that the three runaway stars may have been thrown out of the Orion association by gravitational interaction due to accidentally too close proximity to other massive stars.
Due to its large mass (around 17 times that of the Sun), AE Aurigae will explode as a supernovae and later, as a pulsar, move unusually quickly high above the galactic plane.
literature
- Runaway stars. In: The Brockhaus. Astronomy . 2006, p. 395.
Web link
Individual evidence
- ↑ a b c d e f HD 34078. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed on November 3, 2018 .
- ↑ a b AE Aur. In: VSX. AAVSO, accessed November 3, 2018 .
- ↑ a b Bright Star Catalog
- ↑ a b c d AE Aur. Jim Kaler, accessed November 3, 2018 .
- ↑ Jim Kaler (see web link) assumes after new calculations that only AE Aurigae and My Columbae were part of two binary star systems that once came too close to each other, so that the two runaway stars were thrown away, while the other two stars and the one stayed behind formed today's binary star Nair Al Saif in Orion.