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Iota Aurigae

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ι Aurigae
Location of ι Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga[1]
Right ascension 04h 56m 59.620s[2]
Declination +33° 09′ 57.94″[2]
Apparent magnitude (V) 2.69[3]
Characteristics
Spectral type K3 II–III[4]
U−B color index +1.78[3]
B−V color index +1.53[3]
R−I color index +0.82[4]
Variable type Suspected[4]
Astrometry
Radial velocity (Rv)+17.78[5] km/s
Proper motion (μ) RA: +3.817 mas/yr[2]
Dec.: −17.786 mas/yr[2]
Parallax (π)7.2491±0.3819 mas[2]
Distance450 ± 20 ly
(138 ± 7 pc)
Absolute magnitude (MV)−3.20[1]
Details
Mass7.1±0.7[6] M☉
Radius126[7] R☉
Luminosity3,897±327[7] L☉
Temperature4,059±125[7] K
Metallicity [Fe/H]−0.11[8] dex
Rotational velocity (v sin i)8[9] km/s
Age39.8±4.9[6] Myr
Other designations
Hassaleh, Kabdhilinan, ι Aur, 3 Aurigae, BD+32°855, FK5 181, GC 6029, HD 31398, HIP 23015, HR 1577, SAO 57522[10]
Database references
SIMBADdata

Iota Aurigae is a star in the northern constellation of Auriga. Its name is a Bayer designation that is Latinized from ι Aurigae, abbreviated Iota Aur or ι Aur. The star has the official name Hassaleh, pronounced /ˈhæsəleɪ/.[11] It has an apparent visual magnitude of 2.7,[3] which is bright enough to be readily visible to the naked eye. Parallax measurements give a distance estimate of roughly 450 light-years (140 parsecs) from the Sun.[2] It is drifting further away with a radial velocity of +18 km/s.[5]

Nomenclature

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ι Aurigae (Latinised to Iota Aurigae) is the star's Bayer designation.

It bore the traditional name Al Kab,[12] short for Kabdhilinan /kæbˈdɪlɪnæn/, from the Arabic كعب ذي العنان kaʽb ðīl-ʽinān[13][14] "the ankle[15] of the rein holder (charioteer)".[12] Under the name Alkab, this star is a marker on the astrolabe described by Geoffrey Chaucer in his Treatise on the Astrolabe in 1391.

It bore the novel name Hassaleh in Antonín Bečvář's 1951 atlas. The origin and meaning of the name have not been discovered despite extensive search, and no connection to any language has been discovered.[16] The IAU Working Group on Star Names (WGSN)has approved the proper name Hassaleh for this star.[11]

It is known as 五車一 (the First Star of the Five Chariots) in Chinese.[17]

Properties

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At Iota Aurigae's distance, extinction from interstellar dust is causing a magnitude reduction of about 0.6.[12] Examination of the spectrum yields a stellar classification of K3 II–III, with the luminosity class of 'II–III' indicating this is a evolved hybrid giant star.[4] Since 1943, the spectrum of this star has served as one of the stable anchor points by which other stars are classified.[18] 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.[19]

It 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.[20] This is a suspected variable star.[4]

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. As of 2008, the detection has not been confirmed, though Hekker et al. (2008) listed significant radial velocity variations at periods of 767 and 1586 days.[21][22] It may instead be an oscillating star undergoing non-radial pulsations with a period of about four years.[4]

References

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  1. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
  2. ^ a b c d e 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. ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
  4. ^ a b c d e f Strassmeier, K. G.; et al. (December 2020), "BRITE photometry and STELLA spectroscopy of bright stars in Auriga: Rotation, pulsation, orbits, and eclipses⋆", Astronomy & Astrophysics, 644, id. A104, arXiv:2010.10092, Bibcode:2020A&A...644A.104S, doi:10.1051/0004-6361/202039310.
  5. ^ a b Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304.
  6. ^ a b Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
  7. ^ a b c McDonald, I.; et al. (October 2017), "Fundamental parameters and infrared excesses of Tycho-Gaia stars", Monthly Notices of the Royal Astronomical Society, 471 (1): 770–791, arXiv:1706.02208, Bibcode:2017MNRAS.471..770M, doi:10.1093/mnras/stx1433, ISSN 0035-8711. Iota Aurigae's database entry at VizieR.
  8. ^ a b McWilliam, Andrew (December 1990), "High-resolution spectroscopic survey of 671 GK giants", Astrophysical Journal Supplement Series, 74: 1075–1128, Bibcode:1990ApJS...74.1075M, doi:10.1086/191527, ISSN 0067-0049.
  9. ^ Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago, 239 (1): 1, Bibcode:1970CoAsi.239....1B.
  10. ^ "iot Aur", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2012-01-19.
  11. ^ a b Naming Stars, IAU.org, retrieved 16 December 2017.
  12. ^ a b c Kaler, James B., "Al Kab", Stars, University of Illinois at Urbana-Champaign, archived from the original on 2008-12-10, retrieved 2012-01-18.
  13. ^ Allen, Richard Hinckley (1899), Star-names and their meanings, G. E. Stechert, p. 91.
  14. ^ ʿAbd al-Raḥmān ibn ʿUmar al-Ṣūfī. صور الكواكب الثابتة (Book of Fixed Stars). Manuscript from the National Library of France.
  15. ^ Translation of the Arabic word كعب to English on the Almaany dictionaries website.
  16. ^ Kunitzsch, Paul; Smart, Tim (2006), A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.), Cambridge, Massachusetts: Sky Publishing Company, ISBN 978-1-931559-44-7.
  17. ^ Ridpath, Ian, "Auriga", Star Tales, retrieved 2019-10-10.
  18. ^ Garrison, R. F. (December 1993), "Anchor Points for the MK System of Spectral Classification", Bulletin of the American Astronomical Society, 25: 1319, Bibcode:1993AAS...183.1710G, archived from the original on 2019-06-25, retrieved 2012-02-04.
  19. ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on February 22, 2012, retrieved 2012-01-16.
  20. ^ Kashyap, V.; et al. (August 1994), "X-ray emission on hybrid stars: ROSAT observations of alpha Trianguli Australis and IOTA Aurigae", The Astrophysical Journal, 431 (1): 402–415, Bibcode:1994ApJ...431..402K, doi:10.1086/174494.
  21. ^ Hekker, S.; et al. (2008), "Precise radial velocities of giant stars. IV. A correlation between surface gravity and radial velocity variation and a statistical investigation of companion properties", Astronomy and Astrophysics, 480 (1): 215–222, arXiv:0801.0741, Bibcode:2008A&A...480..215H, doi:10.1051/0004-6361:20078321, S2CID 33442610.
  22. ^ Reffert, S.; et al. (2008), "Two brown dwarfs in resonance around a K3II giant", Extreme Solar Systems, ASP Conference Series, Vol. 398, proceedings of the conference held 25–29 June 2007, at Santorini Island, Greece (PDF), p. 115, archived from the original (PDF) on 18 July 2011, retrieved 18 November 2009.
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