V380 Orionis
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Orion |
| Right ascension | 05h 36m 25.4313s |
| Declination | –06° 42′ 57.704″ |
| Apparent magnitude (V) | 10.2–10.7[1] |
| Characteristics | |
| Spectral type | B9[2] |
| Variable type | None |
| Astrometry | |
| Radial velocity (Rv) | 15.40 km/s |
| Proper motion (μ) | RA: 4.10 ± 3.65 mas/yr Dec.: –3.83 ± 2.62 mas/yr |
| Parallax (π) | 2.86 ± 5.02[3] mas |
| Details | |
| Mass | 2.87[2] M☉ |
| Radius | 3[2] R☉ |
| Luminosity | 100[2] L☉ |
| Temperature | 10500 ± 500[2] K |
| Metallicity | 0.5 |
| Age | 2 ± 1 million years |
| Mass | 1.6[2] M☉ |
| Radius | 2[2] R☉ |
| Luminosity | 0.31[2] L☉ |
| Temperature | 5500 ± 500[2] K |
| Other designations | |
V380 Ori is a young multiple star system located near the Orion Nebula in the constellation Orion, thought to be somewhere between 1 and 3 million years old.[2] One of the component stars appears to have launched a polar jet that helped to clear the keyhole-shaped hole in the surrounding nebula known as NGC 1999.[4] The system is surrounded by a bow shock—the total structure over 17 light-years (5.3 parsecs) across.[5] V380 Orionis is a quadruple star system. The two main stars (until now known collectively as V380 Orionis Aa) are a spectroscopic binary system, the stars orbiting each other over a period of 106 days.[5] The primary is a hot white Herbig Ae/Be star of spectral type B9 that has a surface temperature of 10,500 ± 500 K, and is around 2.87 times as massive and 100 times as luminous as the Sun, and is triple its diameter. The secondary is a T Tauri star that has a surface temperature of 5,500 ± 500 K, and is around 1.6 times as massive and 0.31 times as luminous as the Sun, and is twice its diameter.[2] The two stars are surrounded by a circumstellar disk, lying almost edge-on to observers on earth.[5]
The fourth star (V380 Orionis B) is a small, cool object of spectral type M5 or M6 that is either a red dwarf or brown dwarf, and located around 4000 AU from the main two stars. Reipurth and colleagues calculated that it is most likely in an unstable orbit and that future close approach (periastron) will either bring its orbit closer or fling it out of the system altogether.[5]
The apparent magnitude varies from 10.2 to 10.7.[1]
References
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