Astronomy:AE Aurigae

From HandWiki
Short description: Star in the constellation Auriga
AE Aurigae
Location of AE Aur (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Auriga
Right ascension  05h 16m 18.14933s[1]
Declination +34° 18′ 44.3444″[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±0.6[5] km/s
Proper motion (μ) RA: −4.747[1] mas/yr
Dec.: +43.538[1] mas/yr
Parallax (π)2.5740 ± 0.0340[1] mas
Distance1,270 ± 20 ly
(389 ± 5 pc)
Absolute magnitude (MV)−3.93[6]
Details[6]
Mass19.2±0.3 M☉
Radius6.8±0.5 R☉
Luminosity50,100+4,800
−4,400 L☉
Surface gravity (log g)4.06±0.05 cgs
Temperature33,200±300 K
Rotational velocity (v sin i)9±2 km/s
Age3.98+0.81
−0.70 Myr
Other designations
BD+34°980, GC 6429, HD 34078, HIP 24575, HR 1712, SAO 57816, ADS 3843, CCDM J05163+3419, WDS J05163+3419, IRAS 05130+3415
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, making it faintly visible to the naked eye under very good observing conditions. It was discovered to be a variable star by Daniel Walter Morehouse, in 1923, and received its variable star designation in 1924.[8] 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.

It 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]

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.[10][11]

Companions

Two candidate companion stars have been detected at angular distances of 8.4″ and 0.35″, respectively, but these are thought to be unrelated, optical companions. A new potential companion was discovered using the CHARA array in 2023. In December 2017, it had an angular separation from AE Aurigae of 6.85 mas, and in September 2018 it had an angular separation of 1.74 mas.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  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. ↑ 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. doi:10.1088/0067-0049/193/2/24. Bibcode: 2011ApJS..193...24S. 
  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. doi:10.1002/asna.200710776. Bibcode: 2007AN....328..889K. 
  6. ↑ 6.0 6.1 Aschenbrenner, P.; Przybilla, N.; Butler, K. (2023-03-01). "Quantitative spectroscopy of late O-type main-sequence stars with a hybrid non-LTE method". Astronomy and Astrophysics 671: A36. doi:10.1051/0004-6361/202244906. ISSN 0004-6361. Bibcode: 2023A&A...671A..36A. 
  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. 
  8. ↑ Guthnick, P.; Prager, R.; Heise, E. (November 1924). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten 223 (3): 41–56. doi:10.1002/asna.19242230302. Bibcode: 1924AN....223...41G. 
  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. doi:10.1051/0004-6361:20000014. Bibcode: 2001A&A...365...49H. 
  10. ↑ 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. 
  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): 920–939. doi:10.1086/510481. Bibcode: 2007ApJ...655..920F. 
  12. ↑ Lanthermann, C.; Le Bouquin, J.-B.; Sana, H.; Mérand, A.; Monnier, J. D.; Perraut, K.; Frost, A. J.; Mahy, L. et al. (2023). "Multiplicity of northern bright O-type stars with optical long baseline interferometry". Astronomy & Astrophysics 672: A6. doi:10.1051/0004-6361/202245364. PMID 36974081. Bibcode: 2023A&A...672A...6L. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:AE_Aurigae&oldid=3948364"