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Lambda Aurigae

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Lambda Aurigae

Lambda Aurigae
Diagram showing star positions and boundaries of the Auriga constellation and its surroundings

Location of λ Aurigae (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 05h 19m 08.47420s[1]
Declination +40° 05′ 56.5826″[1]
Apparent magnitude (V) 4.71[2]
Characteristics
Spectral type G1 V[3]
U−B color index +0.13[2]
B−V color index +0.62[2]
R−I color index 0.32
Astrometry
Radial velocity (Rv) 66.5[4] km/s
Proper motion (μ) RA: +518.99±0.26[1] mas/yr
Dec.: −665.06±0.13[1] mas/yr
Parallax (π) 79.17 ± 0.28[1] mas
Distance 41.2 ± 0.1 ly
(12.63 ± 0.04 pc)
Details
Mass 1.081+0.054
−0.029
[5] M
Radius 1.331±0.021[3] R
Luminosity 1.732±0.022[3] L
Surface gravity (log g) 4.02[6] cgs
Temperature 5890±4.3[7] K
Metallicity [Fe/H] +0.01[6] dex
Rotational velocity (v sin i) 2[8] km/s
Age 5.0–7.9[9] Gyr
Other designations
15 Aur, BD+39 1248, FK5 1145, GJ 197, HD 34411, HIP 24813, HR 1729, LFT 403, LHS 1753, LTT 11625, SAO 40233.[10]

Lambda Aurigae (λ Aur, λ Aurigae) is the Bayer designation for a solar analog[11] star in the northern constellation of Auriga.[12] It has the traditional name Al Hurr[13] and is visible to the naked eye with an apparent visual magnitude of 4.71.[2] Based upon parallax measurements made during the Hipparcos mission, it is approximately 41.2 light-years (12.6 parsecs) distant from the Earth.[1]

This is a G-type main sequence star with a stellar classification of G1 V.[3] In terms of composition it is similar to the Sun, while the mass and radius are slightly larger.[5] It is 73% more luminous than the Sun[3] and radiates this energy from its outer atmosphere at an effective temperature of 5890 K.[7] At this heat, the star glows with the yellow hue of a G-type star.[14] It has a low level of surface activity and is a candidate Maunder minimum analog.[15]

Lambda Aurigae has been examined for the presence of excess infrared emission that may indicate the presence of a circumstellar disk of dust, but no significant surplus has been observed.[11] It is a possible member of the Epsilon Indi Moving Group of stars that share a common motion through space. The space velocity components of this star are [U, V, W] = [+76, –39, –6] km/s.[16]

Name

This star is sometimes called by the name Al Hurr, meaning the fawn in Arabic.[13] Lambda Aurigae, along with μ Aur and ρ Aur, were Kazwini's Al Ḣibāʽ (ألحباع), the Tent.[13] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Al Ḣibāʽ were the title for three stars : λ Aur as Al Ḣibāʽ I, μ Aur as Al Ḣibāʽ II and ρ Aur as Al Ḣibāʽ III.[17]

In Chinese, 咸池 (Xián Chí), meaning Pool of Harmony, refers to an asterism consisting of λ Aurigae, ρ Aurigae and HD 36041.[18] Consequently, λ Aurigae itself is known as 咸池三 (Xián Chí sān, English: the Third Star of Pool of Harmony.)[19]

References

  1. ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction",   Note: see VizieR catalogue I/311.
  2. ^ 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),  
  3. ^ a b c d e Boyajian, Tabetha S.; et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal 746 (1): 101,  . See Table 10.
  4. ^ Nordström, B.; et al. (May 2004), "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs", Astronomy and Astrophysics 418: 989–1019,  
  5. ^ a b Takeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series 168 (2): 297–318,  
  6. ^ a b Chen, Y. Q.; et al. (February 2000), "Chemical composition of 90 F and G disk dwarfs", Astronomy and Astrophysics Supplement 141: 491–506,  
  7. ^ a b Kovtyukh, V. V.; et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios",  
  8. ^ Takeda, Yoichi; et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan 57 (1): 13–25,  
  9. ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293,  
  10. ^ "LHS 1753 -- High proper-motion Star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-08-19. 
  11. ^ a b Greaves, J. S.; Wyatt, M. C.; Bryden, G. (August 2009), "Debris discs around nearby solar analogues",  
  12. ^ Kaler, James, "LAMBDA AUR (Lambda Aurigae)", Stars, retrieved 2011-12-11. 
  13. ^ a b c  
  14. ^ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16. 
  15. ^ Lubin, Dan; Tytler, David; Kirkman, David (March 2012), "Frequency of Maunder Minimum Events in Solar-type Stars Inferred from Activity and Metallicity Observations", The Astrophysical Journal Letters 747 (2): L32,  
  16. ^ Kovacs, N.; Foy, R. (August 1978), "A detailed analysis of three stars in the Eggen's Epsilon INDI moving group", Astronomy and Astrophysics 68 (1–2): 27–31,  
  17. ^ Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars (PDF), California Institute of Technology: Jet Propulsion Laboratory, retrieved 2012-08-19. 
  18. ^ (Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
  19. ^ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日

External links

  • Image Lambda Aurigae
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