Lambda Aurigae
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 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 | 5,890 ± 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 | |
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 5,890 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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752v1, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. Note: see VizieR catalogue I/311.
- ↑ 2.0 2.1 2.2 2.3 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99), Bibcode:1966CoLPL...4...99J.
- ↑ 3.0 3.1 3.2 3.3 3.4 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, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101.. See Table 10.
- ↑ 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, arXiv:astro-ph/0405198, Bibcode:2004A&A...418..989N, doi:10.1051/0004-6361:20035959.
- ↑ 5.0 5.1 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, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763.
- ↑ 6.0 6.1 Chen, Y. Q. et al. (February 2000), "Chemical composition of 90 F and G disk dwarfs", Astronomy and Astrophysics Supplement 141: 491–506, arXiv:astro-ph/9912342, Bibcode:2000A&AS..141..491C, doi:10.1051/aas:2000124.
- ↑ 7.0 7.1 Kovtyukh, V. V. et al. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378.
- ↑ 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, Bibcode:2005PASJ...57...13T.
- ↑ 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, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785.
- ↑ "LHS 1753 -- High proper-motion Star", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2012-08-19.
- ↑ 11.0 11.1 Greaves, J. S.; Wyatt, M. C.; Bryden, G. (August 2009), "Debris discs around nearby solar analogues", Monthly Notices of the Royal Astronomical Society 397 (2): 757–762, arXiv:0907.3677, Bibcode:2009MNRAS.397..757G, doi:10.1111/j.1365-2966.2009.15048.x.
- ↑ Kaler, James, "LAMBDA AUR (Lambda Aurigae)", Stars, retrieved 2011-12-11.
- ↑ 13.0 13.1 13.2 Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 91. ISBN 0-486-21079-0. Retrieved 2010-12-12.
- ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, retrieved 2012-01-16.
- ↑ 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, Bibcode:2012ApJ...747L..32L, doi:10.1088/2041-8205/747/2/L32.
- ↑ 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, Bibcode:1978A&A....68...27K.
- ↑ Rhoads, Jack W. (November 15, 1971), Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars, California Institute of Technology: Jet Propulsion Laboratory, retrieved 2012-08-19.
- ↑ (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.
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日
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