AR Aurigae

Last updated
AR Aurigae
ARAurLightCurve.png
A visual band light curve for AR Aurigae, adapted from Johansen (1970) [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Auriga
Right ascension 05h 18m 18.896s [2]
Declination +33° 46′ 02.52″ [2]
Apparent magnitude  (V)6.144 [3]
Characteristics
Spectral type B9V + B9.5V [4]
U−B color index −0.18 [5]
B−V color index −0.06 [5]
Variable type Algol [6]
Astrometry
Radial velocity (Rv)25.4±0.9 [7]  km/s
Proper motion (μ)RA: +15.254 [2]   mas/yr
Dec.: −29.225 [2]   mas/yr
Parallax (π)7.0735 ± 0.0461  mas [2]
Distance 461 ± 3  ly
(141.4 ± 0.9  pc)
Absolute magnitude  (MV)1.11/1.17 [8]
Details
AR Aur A
Mass 2.552±0.008 [4]   M☉
Radius 1.781 [9]   R☉
Luminosity 41 [8]   L☉
Surface gravity (log g)4.33 [4]   cgs
Temperature 10,950±150 [4]   K
Rotational velocity (v sin i)10 [9]  km/s
AR Aur B
Mass 2.367±0.008 [4]   M☉
Radius 1.816 [9]   R☉
Luminosity34 [8]   L☉
Surface gravity (log g)4.28 [4]   cgs
Temperature 10,350±150 [4]   K
Rotational velocity (v sin i)11 [9]  km/s
Other designations
17 Aur, BD+33°1002, HD  34364, HIP  24740, HR  1728, SAO  57858, PPM  70158
Database references
SIMBAD data

AR Aurigae (AR Aur), also known by its Flamsteed designation 17 Aurigae, is a binary star in the constellation Auriga. Based on parallax measurements made by the Hipparcos spacecraft, it is approximately 461 light-years from Earth. [10]

Both components are blue-white B-type main-sequence stars that do not fill their Roche lobes. The system has a mean apparent magnitude of +6.15. However, the orbit of the stars are oriented in such a way that they periodically eclipse each other, so AR Aurigae is a variable star and its brightness varies from magnitude +6.15 to +6.82 with a period of 4.13 days. [6] In 1931, H. N. Pendersen and J. C. Steensgard became the first persons to detect these eclipses. [11] [12] When an eclipse is not occurring, the star will be faintly visible to the naked eye under very good observing conditions.

The primary component of AR Aurigae is known to be a mercury-manganese star, also known as an HgMn star. As the name implies, these stars have over-abundances of the elements mercury and manganese, and also often xenon and other elements. [4] Because AR Aurigae is an eclipsing binary (in fact, it is the only known eclipsing binary with a mercury-manganese star), accurate characterization of its parameters has been made possible. Based on the light-time effect observed from the stars, it is inferred that there is a third star with a mass of 0.54 M☉, orbiting at a separation of 13 AU every 23.7 years. [4]

Related Research Articles

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

Zeta Aurigae, or ζ Aurigae, is a binary star system in the northern constellation of Auriga. Based upon parallax measurements, this system is approximately 860 light-years distant from the Sun. It has a combined apparent visual magnitude of 3.75, which is bright enough to be seen with the naked eye.

<span class="mw-page-title-main">74 Aquarii</span> Triple star system in the constellation Aquarius

74 Aquarii is a triple star system in the constellation of Aquarius. 74 Aquarii is its Flamsteed designation and it also bears the variable star designation HI Aquarii. The combined apparent visual magnitude is 5.8, although it is very slightly variable, and it is located at a distance of 590 light-years from Earth.

<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">HR 2554</span> Star in the constellation Carina

HR 2554, also known as V415 Carinae and A Carinae, is an eclipsing spectroscopic binary of the Algol type in the constellation of Carina whose apparent visual magnitude varies by 0.06 magnitude and is approximately 4.39 at maximum brightness. Its primary is a G-type bright giant star and its secondary is an A-type main-sequence star. It is approximately 553 light-years from Earth.

<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">YZ Cassiopeiae</span> Triple star system in the constellation Cassiopeia

YZ Cassiopeiae is a star system 103.8 parsecs (339 ly) away from Earth, in the constellation Cassiopeia. It comprises three stars: an eclipsing Algol-type binary and a visually fainter star about 3000 AU distant.

<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">22 Vulpeculae</span> Binary star system in the constellation Vulpecula

22 Vulpeculae is a binary star system in the northern constellation Vulpecula. Based on its parallax, it is located some 1,490 light-years away, and it has an apparent magnitude of about 5.2, making it visible to the naked eye. The system is moving closer to the Earth with a heliocentric radial velocity of −23 km/s.

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

1 Persei is an eclipsing binary star in the constellation Perseus. Its uneclipsed apparent magnitude is 5.49. The binary star consists of two B2 type main-sequence stars in a 25.9 day eccentric orbit. The stars are surrounded by a faint cloud of gas visible in mid-infrared, although whether they are the origin of the gas or simply passing through it is unclear.

<span class="mw-page-title-main">Gamma Phoenicis</span> Binary star in the constellation Phoenix

Gamma Phoenicis is a star system in the constellation Phoenix, located around 71.63 parsecs (233.6 ly) distant.

<span class="mw-page-title-main">136 Tauri</span> Star in the constellation Taurus

136 Tauri is a white-hued binary star system in the zodiac constellation of Taurus. It has a combined apparent visual magnitude of 4.56, which is bright enough to be faintly visible to the naked eye. Based upon an annual parallax shift of 7.71±0.22 mas as seen from Earth's orbit, it is located approximately 420 light years from the Sun. The system is moving nearer with a heliocentric radial velocity of −17.2 km/s, and is expected to make its closest approach in 6.5 million years at a distance of 150 ly (45 pc).

<span class="mw-page-title-main">HY Velorum</span> Star in the constellation Vela

HY Velorum is a binary star system in the southern constellation of Vela. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.83. The distance to this system, as estimated from its annual parallax shift of 7.1 mas, is 460 light years. HY Vel most likely forms a gravitationally bound pair with the magnitude 5.45 binary system KT Vel ; both are members of the IC 2391 open cluster. As of 1998, HY Vel and KT Vel had an angular separation of 76.1″ along a position angle of 311°.

<span class="mw-page-title-main">31 Cygni</span> Triple star system in the constellation Cygnus

31 Cygni, also known as ο1 Cygni, Omicron1 Cygni, ο2 Cygni or V695 Cygni, is a ternary star system about 750 light years away in the constellation Cygnus.

<span class="mw-page-title-main">ZZ Boötis</span>

ZZ Boötis is a star system in the constellation Boötes. It varies from magnitude 6.79 to 7.44 over five days. Based on its parallax, measured by the Gaia spacecraft, it is about 350 light-years away.

<span class="mw-page-title-main">CD Crucis</span> Eclipsing binary star system in the constellation Crux

CD Crucis, also known as HD 311884, is an eclipsing binary star system in the constellation Crux. It is around 14,000 light years away near the faint open cluster Hogg 15. The binary contains a Wolf–Rayet star and is also known as WR 47.

Psi<sup>2</sup> Orionis Spectroscopic binary system in the constellation of Orion

Psi2 Orionis a binary star system in the equatorial constellation of Orion. It has an apparent visual magnitude of 4.6, indicating that it is visible to the naked eye. Based upon an annual parallax shift of 2.87 mass, it is roughly 1,100 light years distant from the Sun.

<span class="mw-page-title-main">HR 7484</span> Star in the constellation Cygnus

HR 7484 is a binary star system in the northern constellation of Cygnus. It is dimly visible to the naked eye under good viewing conditions, having an apparent visual magnitude of 5.89. Based upon an annual parallax shift of 24.71, it is located 132 light years away. The system is moving closer with a heliocentric radial velocity of −14 km/s.

<span class="mw-page-title-main">WR 9</span> Spectroscopic binary star system in the constellation Puppis

WR 9 is a spectroscopic binary in the constellation Puppis consisting of a Wolf-Rayet star and a class O star. It is around 12,000 light years away.

<span class="mw-page-title-main">65 Ursae Majoris</span> Star system in the constellation Ursa Major

65 Ursae Majoris, abbreviated as 65 UMa, is a star system in the constellation of Ursa Major. With a combined apparent magnitude of about 6.5, it is at the limit of human eyesight and is just barely visible to the naked eye in ideal conditions. It is about 760 light years away from Earth.

References

  1. ↑ Johansen, K. T. (January 1970). "Light curve and photometric elements of AR Aurigae". Astronomy & Astrophysics. 4: 1–10. Bibcode:1970A&A.....4....1J.
  2. 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.
  3. ↑ Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H.
  4. 1 2 3 4 5 6 7 8 9 Folsom, C. P.; Kochukhov, O.; Wade, G. A.; Silvester, J.; Bagnulo, S. (2010). "Magnetic field, chemical composition and line profile variability of the peculiar eclipsing binary star AR Aur★". Monthly Notices of the Royal Astronomical Society. 407 (4): 2383. arXiv: 1005.3793 . Bibcode:2010MNRAS.407.2383F. doi: 10.1111/j.1365-2966.2010.17057.x . S2CID   13801978.
  5. 1 2 Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N.
  6. 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.
  7. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode:1953GCRV..C......0W.
  8. 1 2 3 Nordstrom, B.; Johansen, K. T. (1994). "Radii and masses for the young star AR Aurigae". Astronomy and Astrophysics. 282: 787. Bibcode:1994A&A...282..787N.
  9. 1 2 3 4 Eker, Z.; Bilir, S.; Soydugan, F.; Gökçe, E. Yaz; Soydugan, E.; Tüysüz, M.; Şenyüz, T.; Demircan, O. (2014). "The Catalogue of Stellar Parameters from the Detached Double-Lined Eclipsing Binaries in the Milky Way". Publications of the Astronomical Society of Australia. 31. arXiv: 1403.1583 . Bibcode:2014PASA...31...24E. doi:10.1017/pasa.2014.17. S2CID   119238300.
  10. ↑ 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. Vizier catalog entry
  11. ↑ Pedersen, H. N.; Steensgaard, J. C. (1931). "Title Not Known". Beobachtungs-Zirkular. 13: 70.
  12. ↑ Nassau, J. J. (July 1936). "Light elements and orbit of AR Aurigae". Astronomical Journal. 45 (1051): 137–140. Bibcode:1936AJ.....45..137N. doi:10.1086/105358 . Retrieved 29 November 2024.
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.