V380 Orionis

From Wikipedia, the free encyclopedia
Jump to: navigation, search
V380 Orionis
Observation data
Epoch J2000      Equinox J2000
Constellation Orion
Right ascension 05h 36m 25.43150s[1]
Declination –06° 42′ 57.6855″[1]
Apparent magnitude (V) 10.2–10.7[2]
Spectral type B9[3]
Variable type Orion variable[4]
Radial velocity (Rv) 15.40 km/s
Proper motion (μ) RA: 4.10 ± 3.65[1] mas/yr
Dec.: –3.83 ± 2.62[1] mas/yr
Parallax (π) 2.86 ± 5.02[1] mas
Mass 2.87 M
Radius R
Luminosity 100 L
Temperature 10500 ± 500 K
Metallicity 0.5
Age 2 ± 1 million years
Mass 1.6 M
Radius R
Luminosity 0.31 L
Temperature 5500 ± 500 K
Other designations
V380 Ori, BD−06°1253, HIP 26327, WDS J05365-0643
Database references

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.[3] 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.[5] The system is surrounded by a bow shock—the total structure over 17 light-years (5.3 parsecs) across.[6] 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.[6] 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.[3] The two stars are surrounded by a circumstellar disk, lying almost edge-on to observers on earth.[6]

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.[6]

The apparent magnitude varies from 10.2 to 10.7.[2]


  1. ^ a b c d e van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752Freely accessible. doi:10.1051/0004-6361:20078357. Vizier catalog entry
  2. ^ a b de Winter, D.; van den Ancker, M. E.; Maira, A.; Thé, P. S.; Djie, H. R. E. Tjin A.; Redondo, I.; et al. (2001). "A photometric catalogue of southern emission-line stars". Astronomy and Astrophysics. 380: 609–14. Bibcode:2001A&A...380..609D. arXiv:astro-ph/0110495Freely accessible. doi:10.1051/0004-6361:20011476. 
  3. ^ a b c d Alecian, E.; Wade, G. A.; Catala, C.; Bagnulo, S.; Böhm, T.; Bouret, J.-C.; et al. (2009). "Magnetism and binarity of the Herbig Ae star V380 Ori†". Monthly Notices of the Royal Astronomical Society. 400 (1): 354–68. Bibcode:2009MNRAS.400..354A. arXiv:0907.5113Freely accessible. doi:10.1111/j.1365-2966.2009.15460.x. 
  4. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S. 
  5. ^ "PIA13109: Big Hole Revealed in Infrared". Photojournal. Jet Propulsion Laboratory, California Institute of Technology/NASA. 11 May 2010. Retrieved 19 May 2010. 
  6. ^ a b c d Reipurth, Bo; Bally, John; Aspin, Colin; Connelley, M. S.; Geballe, T. R.; Kraus, Stefan; et al. (2013). "HH 222: A Giant Herbig-Haro Flow from the Quadruple System V380 Ori". The Astronomical Journal. 146 (5): 11. Bibcode:2013AJ....146..118R. doi:10.1088/0004-6256/146/5/118. 118.