Astronomy:AE Aurigae

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Short description: Star in the constellation Auriga
AE Aurigae
Auriga constellation map.svg
Red circle.svg
Location of AE Aur (circled)
Observation data
Equinox J2000.0]] (ICRS)
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
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±0.6[4] km/s
Proper motion (μ) RA: -4.440[5] mas/yr
Dec.: 43.368[5] mas/yr
Parallax (π)2.4642 ± 0.0660[5] mas
Distance1,320 ± 40 ly
(410 ± 10 pc)
Details[6]
Mass23 M☉
Radius7.47 R☉
Luminosity59,000 L☉
Surface gravity (log g)4.0 cgs
Temperature33,000 K
Rotational velocity (v sin i)25[6] km/s
Other designations
Database references
SIMBADdata

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

Description

Hipparcos light curves for AE Aurigae. The main plot shows the long-term variation, and the inset plot shows the variation folded over a period of 213.7 days. Adapted from Marchenko et al. (1998)[7]

AE Aurigae is a blue O-type main sequence star 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 1,300 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.[8]

Flaming star nebula
Nebula IC 405 around AE Aurigae

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.[9][10]

Companions

Possibly due to its runaway star nature, AE Aurigae has no physical companion stars, although some nearby stars have been erroneously identified as ones. A theoretical companion 1000 AU (0.016 light-years) away from AE Aurigae would have an angular separation of less than 2.5 arcseconds and would probably be lost in the star's glare.[citation needed]

References

  1. ↑ 1.0 1.1 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 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. ↑ 3.0 3.1 Samus, N. N. 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. ↑ 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. doi:10.1002/asna.200710776. Bibcode: 2007AN....328..889K. 
  5. ↑ 5.0 5.1 5.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. 
  6. ↑ 6.0 6.1 Martins, F.; Hervé, A.; Bouret, J.-C.; Marcolino, W.; Wade, G. A.; Neiner, C.; Alecian, E.; Grunhut, J. et al. (2015). "The MiMeS survey of magnetism in massive stars: CNO surface abundances of Galactic O stars". Astronomy & Astrophysics 575: A34. doi:10.1051/0004-6361/201425173. Bibcode: 2015A&A...575A..34M. 
  7. ↑ Marchenko, S. V.; Moffat, A. F. J.; van der Hucht, K. A.; Seggewiss, W.; Schrijver, H.; Stenholm, B.; Lundström, I.; Setia Gunawan, D. Y. A. et al. (March 1998). "Wolf-Rayet stars and O-star runaways with HIPPARCOS II. Photometry". Astronomy & Astrophysics 331: 1022–1036. Bibcode: 1998A&A...331.1022M. https://ui.adsabs.harvard.edu/abs/1998A&A...331.1022M. Retrieved 29 October 2021. 
  8. ↑ 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. doi:10.1051/0004-6361:20000014. Bibcode: 2001A&A...365...49H. 
  9. ↑ López-Santiago, J.; Miceli, M.; Del Valle, M. V.; Romero, G. E.; Bonito, R.; Albacete-Colombo, J. F.; Pereira, V.; De Castro, E. et al. (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 (1): L6. doi:10.1088/2041-8205/757/1/L6. Bibcode: 2012ApJ...757L...6L. 
  10. ↑ 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): 920–939. doi:10.1086/510481. Bibcode: 2007ApJ...655..920F. 

External links



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