AE Aurigae

AE Aurigae


Location of AE Aur (circled)

Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 05h 16m 18.15000s[1]
Declination +34° 18′ 44.3455″[1]
Apparent magnitude (V) 5.96[2] (5.78 - 6.08[3])
Characteristics
Spectral type O9.5V[4]
U−B color index −0.70[2]
B−V color index +0.22[2]
Variable type Orion variable[3]
Astrometry
Radial velocity (Rv)56.70[5] km/s
Proper motion (μ) RA: -3.58[1] mas/yr
Dec.: 43.73[1] mas/yr
Parallax (π)2.24 ± 0.74[1] mas
Distance534[6] pc
Absolute magnitude (MV)−3.92[7]
Details[7]
Mass23 M☉
Radius7.47 R☉
Luminosity59,000 L☉
Surface gravity (log g)4.0 cgs
Temperature33,000 K
Rotational velocity (v sin i)25[8] km/s
Other designations
GC 6429, IDS 05097+3412, GCRV 3123, IRAS 05130+3415, TYC 2398-894-1, ADS 3843, UBV M 10749, AG+34°542, GOS G172.08-02.26 01, uvby98 100034078 ABV, GSC 02398-00894, VDB 34, BD+34°980, HD 34078, PLX 1190, CCDM J05163+3419, PPM Star Catalogue 70112, AAVSO 0509+34, HIP 24575, ROT 748, WDS J05163+3419, CGO 80, SAO 57816, CSI+34 980 1, HR 1712
Database references
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)
Database references
SIMBADdata

AE Aurigae (AE Aur) is a runaway star in the constellation Auriga; it lights the Flaming Star Nebula.

Description

Flaming star nebula
Flaming star nebula around AE Aur

AE Aurigae is a blue O-type main sequence dwarf with a mean apparent magnitude of +6.0. It is classified as an Orion type variable star and its brightness varies irregularly between magnitudes +5.78 and +6.08. It is approximately 1,700 light-years from Earth.

AE Aur is a runaway star that might have been ejected during a collision of two binary star groups. This collision, which also is credited with ejecting Mu Columbae and possibly 53 Arietis, has been traced to the Trapezium cluster in the Orion Nebula two million years ago. The binary Iota Orionis may have been the other half of this collision.[9]

AE Aur is seen to light up the Flaming Star nebula, but it was not formed within it. Instead it is passing through the nebula at high speed and producing a violent bow shock and high energy electromagnetic radiation.[10][11]

Companions

AE Aur has a close 8th magnitude companion component B.

There is also a more distant companion HD 34042, sometimes called component C, which has a spectral type of A5.

See also

References

  1. 1 2 3 4 5 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 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.
  4. ↑ Sota, A.; Maíz Apellániz, J.; Walborn, N. R.; Alfaro, E. J.; Barbá, R. H.; Morrell, N. I.; Gamen, R. C.; Arias, J. I. (2011). "The Galactic O-Star Spectroscopic Survey. I. Classification System and Bright Northern Stars in the Blue-violet at R ~ 2500". The Astrophysical Journal Supplement 193 (2): 24. arXiv:1101.4002. Bibcode:2011ApJS..193...24S. doi:10.1088/0067-0049/193/2/24.
  5. ↑ Kharchenko, N. V.; Scholz, R.-D.; Piskunov, A. E.; Röser, S.; Schilbach, E. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten 328 (9): 889. arXiv:0705.0878. Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776.
  6. ↑ Meurs, E. J. A.; Fennell, G.; Norci, L. (2005). "X-Ray Counterparts of Runaway Stars". The Astrophysical Journal 624: 307. Bibcode:2005ApJ...624..307M. doi:10.1086/428874.
  7. 1 2 Martins, F.; Schaerer, D.; Hillier, D. J.; Meynadier, F.; Heydari-Malayeri, M.; Walborn, N. R. (2005). "On stars with weak winds: The Galactic case". Astronomy and Astrophysics 441 (2): 735. arXiv:astro-ph/0507278. Bibcode:2005A&A...441..735M. doi:10.1051/0004-6361:20052927.
  8. ↑ Martins, F.; Hervé, A.; Bouret, J.-C.; Marcolino, W.; Wade, G. A.; Neiner, C.; Alecian, E.; Grunhut, J.; Petit, V. (2015). "The MiMeS survey of magnetism in massive stars: CNO surface abundances of Galactic O stars". Astronomy & Astrophysics 575: A34. arXiv:1411.4420. Bibcode:2015A&A...575A..34M. doi:10.1051/0004-6361/201425173.
  9. ↑ Hoogerwerf, R.; De Bruijne, J. H. J.; De Zeeuw, P. T. (2001). "On the origin of the O and B-type stars with high velocities. II. Runaway stars and pulsars ejected from the nearby young stellar groups". Astronomy and Astrophysics 365 (2): 49. arXiv:astro-ph/0010057. Bibcode:2001A&A...365...49H. doi:10.1051/0004-6361:20000014.
  10. ↑ López-Santiago, J.; Miceli, M.; Del Valle, M. V.; Romero, G. E.; Bonito, R.; Albacete-Colombo, J. F.; Pereira, V.; De Castro, E.; Damiani, F. (2012). "AE Aurigae: First Detection of Non-thermal X-Ray Emission from a Bow Shock Produced by a Runaway Star". The Astrophysical Journal Letters 757: L6. arXiv:1208.6511. Bibcode:2012ApJ...757L...6L. doi:10.1088/2041-8205/757/1/L6.
  11. ↑ France, Kevin; McCandliss, Stephan R.; Lupu, Roxana E. (2007). "A Cometary Bow Shock and Mid-Infrared Emission Variations Revealed in Spitzer Observations of HD 34078 and IC 405". The Astrophysical Journal 655 (2): 920. arXiv:astro-ph/0610953. Bibcode:2007ApJ...655..920F. doi:10.1086/510481.

External links

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