AR Aurigae

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Template:Short description

AR Aurigae
File: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 Template:RA[2]
Declination Template:DEC[2]
Apparent magnitude (V) 6.144[3]
Characteristics
Spectral type B9V + B9.5V[4]
U−B Template:Engvar −0.18[5]
B−V Template:Engvar −0.06[5]
Variable type Algol[6]
Astrometry
Radial velocity (Rv)Script error: No such module "val".[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]
DistanceTemplate:Rnd ± Template:Rnd ly
(Template:Rnd ± Template:Rnd pc)
Absolute magnitude (MV)1.11/1.17[8]
Details
AR Aur A
MassScript error: No such module "val".[4] Template:Solar mass
Radius1.781[9] Template:Solar radius
Luminosity41[8] Template:Solar luminosity
Surface gravity (log g)4.33[4] cgs
TemperatureScript error: No such module "val".[4] K
Rotational velocity (v sin i)10[9] km/s
AR Aur B
MassScript error: No such module "val".[4] Template:Solar mass
Radius1.816[9] Template:Solar radius
Luminosity34[8] Template:Solar luminosity
Surface gravity (log g)4.28[4] cgs
TemperatureScript error: No such module "val".[4] K
Metallicity [Fe/H]{{{metal_fe2}}} dex
Rotational velocity (v sin i)11[9] km/s
Other designations
Template:Odlist
Database references
SIMBADdata

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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 Template:Solar mass, orbiting at a separation of 13 AU every 23.7 years.[4]

References

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  1. ↑ Script error: No such module "Citation/CS1".
  2. ↑ a b c d e Template:Cite Gaia DR3
  3. ↑ Script error: No such module "Citation/CS1".
  4. ↑ a b c d e f g h i Script error: No such module "Citation/CS1".
  5. ↑ a b Script error: No such module "Citation/CS1".
  6. ↑ a b Script error: No such module "Citation/CS1".
  7. ↑ Script error: No such module "Citation/CS1".
  8. ↑ a b c Script error: No such module "Citation/CS1".
  9. ↑ a b c d Script error: No such module "Citation/CS1".
  10. ↑ Script error: No such module "Citation/CS1". Vizier catalog entry
  11. ↑ Script error: No such module "Citation/CS1".
  12. ↑ Script error: No such module "Citation/CS1".

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External links

Template:Stars of Auriga

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