Iota Aurigae

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Iota Aurigae
Diagram showing star positions and boundaries of the Auriga constellation and its surroundings
Cercle rouge 100%.svg

Location of ι Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 04h 56m 59.62109s[1]
Declination +33° 09′ 57.9585″[1]
Apparent magnitude (V) 2.69[2]
Characteristics
Spectral type K3 II[3]
U−B color index +1.78[2]
B−V color index +1.53[2]
R−I color index 0.82[citation needed]
Variable type Suspected[4]
Astrometry
Radial velocity (Rv) +17.78[5] km/s
Proper motion (μ) RA: +6.79[1] mas/yr
Dec.: -14.88[1] mas/yr
Parallax (π) 6.61 ± 0.38[1] mas
Distance 490 ± 30 ly
(151 ± 9 pc)
Details
Mass 7.1 ± 0.7[6] M☉
Radius 127[7] R☉
Surface gravity (log g) 1.74[8] cgs
Temperature 4,160[8] K
Metallicity [Fe/H] –0.11[8] dex
Rotational velocity (v sin i) 8[9] km/s
Age 39.8 ± 4.9[6] Myr
Other designations
Hassaleh, Kabdhilinan, 3 Aurigae, HR 1577, HD 31398, BD+32°855, FK5 181, HIP 23015, SAO 57522, GC 6029.[10]

Iota Aurigae (ι Aur, ι Aurigae) is a star in the northern constellation of Auriga. It has the traditional name Al Kab,[11] short for Kabdhilinan, from the Arabic الكعب ذي العنان al-kacb ðīl-cinān[12] "the shoulder of the rein holder (charioteer)".[11] Under the name Alkab, this star is a marker on the astrolabe described by Geoffrey Chaucer in his Treatise on the Astrolabe in 1391. In Antonín Bečvář's atlas it has the traditional name Hassaleh. It is known as 五車一 (the First Star of the Five Chariots) in Chinese.[citation needed]

This star has an apparent visual magnitude of 2.7,[2] which is bright enough to be readily visible to the naked eye. Parallax measurements give a distance estimate of roughly 490 light-years (150 parsecs) from the Earth. At this distance, extinction from interstellar dust is causing a magnitude reduction of about 0.6.[11] Examination of the spectrum yields a stellar classification of K3 II,[3] with the luminosity class of 'II' indicating this is a category of evolved star known as a bright giant. Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[13] The effective temperature of the outer envelope is 4,160 K,[8] which is cooler than the Sun's effective temperature and gives Iota Aurigae the orange hue of a K-type star.[14]

This star is a weak X-ray emitter with an X-ray luminosity of about 1.8 × 1027 ergs s−1. This emission is most likely coming from transient loops of plasma in Iota Aurigae's outer atmosphere, which have a temperature of around 3 million K.[15] This is a suspected variable star, although this variability remains unconfirmed.[4]

Unconfirmed substellar companions

During the Extreme Solar Systems conference held on June 25–29, 2007, in Santorini, Greece, Reffert et al. announced the detection of two substellar objects orbiting Iota Aurigae in 2:1 resonance. Such companions would be brown dwarfs with orbital periods of approximately 2 and 4 years. No minimum mass for the candidates was provided. So far the detection has not been confirmed, though Hekker et al. (2008) listed significant radial velocity variations at periods of 767 and 1586 days.[16][17]

References

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External links

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  11. ↑ 11.0 11.1 11.2 Lua error in package.lua at line 80: module 'strict' not found.
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