AE Aurigae

Last updated
AE Aurigae
Auriga constellation map.svg
Red circle.svg
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±0.6 [5]  km/s
Proper motion (μ)RA: -4.440 [6]   mas/yr
Dec.: 43.368 [6]   mas/yr
Parallax (π)2.4642 ± 0.0660  mas [6]
Distance 1,363±79  ly
(418±24  pc) [7]
Details [7]
Mass 19.2±0.3  M☉
Radius 6.8±0.5  R☉
Luminosity 50,100+4,800
−4,400  L☉
Surface gravity (log g)4.06±0.05  cgs
Temperature 33,200±300  K
Rotational velocity (v sin i)9±2 km/s
Age 3.98+0.81
−0.70  Myr
Other designations
AG+34°542, BD+34°980, GC  6429, HD  34078, HIP  24575, HR  1712, SAO  57816, ADS  3843, CCDM J05163+3419, WDS J05163+3419, GCRV  3123, IRAS 05130+3415
Database references
SIMBAD data

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

Contents

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) AEAurLightCurve.png
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)

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. [9] 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. [10]

Nebula IC 405 around AE Aurigae IC405 Flaming Star Nebula from the Mount Lemmon SkyCenter Schulman Telescope courtesy Adam Block.jpg
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. [11] [12]

Related Research Articles

<span class="mw-page-title-main">9 Aurigae</span> Multiple star system in the constellation Auriga

9 Aurigae is a star system in Auriga (constellation). It has an apparent magnitude of about 5, making it visible to the naked eye in many suburban skies. Parallax estimates made by the Hipparcos spacecraft put it at about 86 light-years from the solar system, although individual Gaia Data Release 3 parallaxes place all three components at 88 light years.

<span class="mw-page-title-main">RT Aurigae</span> Star in the constellation Auriga

RT Aurigae is a yellow supergiant variable star in the constellation Auriga, about 1,500 light years from Earth.

<span class="mw-page-title-main">Mu Columbae</span> Star in the constellation Columba

Mu Columbae is a star in the constellation of Columba. It is one of the few O-class stars that are visible to the unaided eye. The star is known to lie approximately 1,900 light years from the Solar System.

<span class="mw-page-title-main">CS Camelopardalis</span> Binary star in the constellation Camelopardalis

CS Camelopardalis is a binary star in reflection nebula VdB 14, in the constellation Camelopardalis.

<span class="mw-page-title-main">Kappa Cassiopeiae</span> Star in the constellation Cassiopeia

Kappa Cassiopeiae is a star in the constellation Cassiopeia.

<span class="mw-page-title-main">1 Vulpeculae</span> Star in the constellation Vulpecula

1 Vulpeculae is a class B4IV star in the constellation Vulpecula. Its apparent magnitude is 4.77 and it is approximately 780 light years away based on parallax.

<span class="mw-page-title-main">12 Vulpeculae</span> Star in the constellation Vulpecula

12 Vulpeculae is a star in the northern constellation of Vulpecula, located approximately 630 light years away based on parallax. It has the variable star designation V395 Vul; 12 Vulpeculae is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued star with a baseline apparent visual magnitude of 4.928. It is moving closer to the Earth with a heliocentric radial velocity of -25 km/s.

<span class="mw-page-title-main">LY Aurigae</span> Binary star in the constellation Auriga

LY Aurigae is a multiple star system in the constellation Auriga. It is an eclipsing binary variable star, dropping in brightness by 0.7 magnitudes every 4 days. The system is around a thousand light years away in the Auriga OB1 stellar association.

<span class="mw-page-title-main">NO Aurigae</span> Star in the constellation Auriga

NO Aurigae is a pulsating variable star in the constellation Auriga. It is an unusually-luminous asymptotic giant branch star about 3,500 light years away.

<span class="mw-page-title-main">V Hydrae</span> Variable star in the constellation Hydra

V Hydrae is a carbon star in the constellation Hydra. To date perhaps uniquely in our galaxy it has plasma ejections/eruptions on a grand scale that could be caused by its near, unseen companion.

<span class="mw-page-title-main">RT Carinae</span> Star in the constellation Carina

RT Carinae, also known as CD-58 3538, is a red supergiant and a variable star, located 7,000 light years away in the constellation Carina. It is in the Carina Nebula. The average apparent magnitude of +8.55, too faint to be visible to the naked eye.

<span class="mw-page-title-main">13 Monocerotis</span> Star in the constellation Monoceros

13 Monocerotis is a class A0 Ib star in the constellation Monoceros. Its apparent magnitude is 4.5 and it is approximately 780 parsecs (2,500 ly) away.

<span class="mw-page-title-main">QZ Puppis</span> Star in the constellation Puppis

QZ Puppis is a class B2.5V star in the constellation Puppis. Its apparent magnitude is 4.5 and it is approximately 650 light years away based on parallax.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

<span class="mw-page-title-main">PV Cephei</span> Star in the constellation Cepheus

PV Cephei is a variable star of Orion type located in the constellation of Cepheus at a distance of about 1,100 light-years from Earth. In visible light it varies in brightness from magnitude 17 to 19, making it far too faint to be seen by the naked eye.

<span class="mw-page-title-main">10 Persei</span> Blue supergiant star in the constellation Perseus

10 Persei is a blue supergiant star in the constellation Perseus. Its apparent magnitude is 6.26 although it is slightly variable.

<span class="mw-page-title-main">HD 87643</span> Binary star system in the constellation Carina

HD 87643 is a B[e] class binary star embedded in a reflection nebula.

<span class="mw-page-title-main">HD 65750</span> Star in the constellation Carina

HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.

<span class="mw-page-title-main">RY Tauri</span> Star in the constellation Taurus

RY Tauri is a young T Tauri star in the constellation of Taurus about 450 light years away, belonging to the Taurus Molecular Cloud. It is more massive than typical T Tauri stars, and may be an intermediate between this class and the Herbig Ae/Be star type.

<span class="mw-page-title-main">HD 150193</span> Young binary star system in the constellation Ophiuchus

HD 150193 is a binary star system in the constellation of Ophiuchus. The primary star was identified as a Herbig Ae/Be star with a strong solar wind, losing approximately a tenth of solar mass per million years. It does host a very small debris disk, likely due to disk truncation by the nearby stellar companion. The disk is inclined 38±9° to the plane of sky. It appears to be highly evolved and asymmetric, with indications of flattening and grains growth.

References

  1. 1 2 Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv: 0708.1752 . Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID   18759600.
  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. S2CID   119248206.
  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. S2CID   119323941.
  6. 1 2 3 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 .
  7. 1 2 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. arXiv: 2301.09462 . Bibcode:2023A&A...671A..36A. doi:10.1051/0004-6361/202244906. ISSN   0004-6361.
  8. ↑ 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.; Sutantyo, W.; van den Heuvel, E. P. J.; De Cuyper, J. P.; Gómez, A. E. (March 1998). "Wolf-Rayet stars and O-star runaways with HIPPARCOS II. Photometry". Astronomy & Astrophysics. 331: 1022–1036. Bibcode:1998A&A...331.1022M . Retrieved 29 October 2021.
  9. ↑ Guthnick, P.; Prager, R.; Heise, E. (November 1924). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten. 223 (3): 41–56. Bibcode:1924AN....223...41G. doi:10.1002/asna.19242230302 . Retrieved 28 November 2024.
  10. ↑ 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. S2CID   18970167.
  11. ↑ 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 (1): L6. arXiv: 1208.6511 . Bibcode:2012ApJ...757L...6L. doi:10.1088/2041-8205/757/1/L6. S2CID   37792833.
  12. ↑ 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. arXiv: astro-ph/0610953 . Bibcode:2007ApJ...655..920F. doi:10.1086/510481. S2CID   16963366.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.