AE Aurigae

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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 18.14933s [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  mas/yr [1]
Dec.: +43.538  mas/yr [1]
Parallax (π)2.5740 ± 0.0340  mas [1]
Distance 1,360±260  ly
(418±24  pc) [6]
Details [6]
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. [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]

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. [10] [11]

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">UU Aurigae</span> Star in the constellation of Auriga

UU Aurigae is a carbon star in the constellation Auriga. It is approximately 341 parsecs from Earth. It is a variable star that is occasionally bright enough to be seen by the naked eye under excellent observing conditions.

<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. Although its brightness is variable, it as consistently visible to the naked eye under good observing conditions.

<span class="mw-page-title-main">59 Aurigae</span> Star in the constellation Auriga

59 Aurigae, often abbreviated as 59 Aur, is a star in the constellation Auriga. Its baseline apparent magnitude is 6.1, meaning it can just barely be seen with the naked eye as a dim, yellow-white hued star. Based on parallax measurements, it is located about 483 light-years away from the Sun.

<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">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">V420 Aurigae</span> Star in the constellation Auriga

V420 Aurigae is a high-mass star with an inferred compact companion. Closely orbiting each other every 0.8 days, they are a source of X-ray emission.

<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. It is a 6th magnitude star faintly visible to the naked eye under very good observing conditions.

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

AB Aurigae is a young Herbig Ae star in the Auriga constellation. It is located at a distance of approximately 509 light years from the Sun based on stellar parallax. This pre-main-sequence star has a stellar classification of A0Ve, matching an A-type main-sequence star with emission lines in the spectrum. It has 2.4 times the mass of the Sun and is radiating 38 times the Sun's luminosity from its photosphere at an effective temperature of 9,772 K. The radio emission from the system suggests the presence of a thermal jet originating from the star with a velocity of 300 km s−1. This is causing an estimated mass loss of 1.7×10−8 M☉ yr−1.

<span class="mw-page-title-main">V4381 Sagittarii</span> Star in the constellation Sagittarius

V4381 Sagittarii is a variable star in the constellation Sagittarius. A white supergiant of spectral type A2/A3Iab, it is an Alpha Cygni variable that varies between apparent photographic magnitudes 6.57 and 6.62. Its visual apparent magnitude is about 6.54.

<span class="mw-page-title-main">1 Camelopardalis</span> Double star system in the constellation Camelopardalis

1 Camelopardalis is a double star system in the constellation Camelopardalis. Its combined apparent magnitude is 5.56 and it is approximately 800 parsecs (2,600 ly) away. It is faintly visible to the naked eye under good observing conditions.

<span class="mw-page-title-main">WR 24</span> Wolf-Rayet star in the constellation Carina

WR 24 is a Wolf-Rayet star in the constellation Carina. It is one of the most luminous stars known. At the edge of naked eye visibility it is also one of the brightest Wolf Rayet stars in the sky.

<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">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">Y Centauri</span> Variable star in the constellation Centaurus

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

<span class="mw-page-title-main">9 Persei</span> Blue supergiant star in the constellation Perseus

9 Persei is a single variable star in the northern constellation Perseus, located around 4,300 light years away from the Sun. It has the Bayer designation i Persei; 9 Persei is the Flamsteed designation. This body is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of about 5.2. It is moving closer to the Sun with a heliocentric radial velocity of −15.2 km/s. The star is a member of the Perseus OB1 association of co-moving stars.

<span class="mw-page-title-main">HD 316285</span> Star in the constellation Sagittarius

HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the Galactic Center.

<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">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 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  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 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.
  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.; 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.
  8. ↑ 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.
  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. S2CID   18970167.
  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 (1): L6. arXiv: 1208.6511 . Bibcode:2012ApJ...757L...6L. doi:10.1088/2041-8205/757/1/L6. S2CID   37792833.
  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. arXiv: astro-ph/0610953 . Bibcode:2007ApJ...655..920F. doi:10.1086/510481. S2CID   16963366.
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