Lambda Aurigae: Difference between revisions
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==Name== |
==Name== |
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This star may have been called by the name ''Al Hurr'', meaning ''the fawn'' in Arabic.<ref name=allen1962/> Lambda Aurigae, along with [[Mu Aurigae|μ Aur]] and [[ |
This star may have been called by the name ''Al Hurr'', meaning ''the fawn'' in Arabic.<ref name=allen1962/> Lambda Aurigae, along with [[Mu Aurigae|μ Aur]] and [[Sigma Aurigae|σ Aur]], were Kazwini's ''Al Ḣibāʽ'' ('''ألحباع'''), the Tent.<ref name=allen1962/> 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'', [[Mu Aurigae|μ Aur]] as ''Al Ḣibāʽ II'' and [[Sigma Aurigae|σ Aur]] as ''Al Ḣibāʽ III''.<ref name=rhoads1971/> |
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In [[Chinese astronomy|Chinese]], {{lang|zh|咸池}} ({{lang|zh-Latn|Xián Chí}}), meaning ''[[Net (Chinese constellation)|Pool of Harmony]]'', refers to an asterism consisting of λ Aurigae, [[Rho Aurigae|ρ Aurigae]] and [[HD 36041]].<ref>{{in lang|zh}} ''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}}.</ref> Consequently, the [[Chinese star names|Chinese name]] for λ Aurigae itself is {{lang|zh|咸池三}} ({{lang|zh-Latn|Xián Chí sān}}, {{lang-en|the Third Star of Pool of Harmony}}.)<ref name=sb0>{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0607/ap060713.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日]</ref> |
In [[Chinese astronomy|Chinese]], {{lang|zh|咸池}} ({{lang|zh-Latn|Xián Chí}}), meaning ''[[Net (Chinese constellation)|Pool of Harmony]]'', refers to an asterism consisting of λ Aurigae, [[Rho Aurigae|ρ Aurigae]] and [[HD 36041]].<ref>{{in lang|zh}} ''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}}.</ref> Consequently, the [[Chinese star names|Chinese name]] for λ Aurigae itself is {{lang|zh|咸池三}} ({{lang|zh-Latn|Xián Chí sān}}, {{lang-en|the Third Star of Pool of Harmony}}.)<ref name=sb0>{{in lang|zh}} [http://aeea.nmns.edu.tw/2006/0607/ap060713.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日]</ref> |
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==Observation== |
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From [[Earth]], Lambda Aurigae has an [[apparent magnitude]] of 4.71. The closest large neighboring star to Lambda Aurigae is [[Capella]], located {{Convert|4.5|ly|pc|abbr=off|lk=on}} away.<ref name="SolStation"/> Hypothetically viewed from Lambda Aurigae, Capella's quadruple [[star system]] would have an apparent magnitude of approximately -5.48,<ref name="Wolfram"/> about 40 times brighter than [[Sirius]] can be seen at maximum brightness from Earth.<ref>{{cite web | title=Magnitude Arithmetic|url=http://www.caglow.com/info/wtopic/mag-arith | work=Weekly Topic | publisher=Caglow | access-date=10 February 2023 | archive-url=https://web.archive.org/web/20120201203951/http://www.caglow.com/info/wtopic/mag-arith | archive-date=1 February 2012|url-status=live}}</ref> |
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==References== |
==References== |
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| doi=10.1086/427854 | bibcode=2005AJ....129.1483L |
| doi=10.1086/427854 | bibcode=2005AJ....129.1483L |
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| arxiv=astro-ph/0412070 | s2cid=2603568 | postscript=. }}</ref> |
| arxiv=astro-ph/0412070 | s2cid=2603568 | postscript=. }}</ref> |
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<ref name="SolStation">{{cite web | url=http://www.solstation.com/stars2/capella4.htm|title = Capella 4 | publisher = SolStation |
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| access-date = 10 February 2023}}</ref> |
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<ref name="Wolfram">{{cite web | url=https://www.wolframalpha.com/widgets/view.jsp?id=aa35819112b597d719cc24ba31e63c34|title = Combined apparent magnitude of 2 stars | publisher = WolframΑlpha |
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| access-date = 10 February 2023}}</ref> |
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Revision as of 14:25, 20 August 2023
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 19m 08.47546s[1] |
Declination | +40° 05′ 56.5896″[1] |
Apparent magnitude (V) | 4.71[2] |
Characteristics | |
Spectral type | G1 V[3] or G1.5 IV-V Fe-1[4] |
U−B color index | +0.13[2] |
B−V color index | +0.62[2] |
R−I color index | 0.32 |
Astrometry | |
Radial velocity (Rv) | +66.53±0.14[1] km/s |
Proper motion (μ) | RA: +520.581[1] mas/yr Dec.: −664.826[1] mas/yr |
Parallax (π) | 80.1054 ± 0.2158 mas[1] |
Distance | 40.7 ± 0.1 ly (12.48 ± 0.03 pc) |
Absolute magnitude (MV) | 4.20[5] |
Details | |
Mass | 1.081+0.054 −0.029[6] M☉ |
Radius | 1.331±0.021[3] R☉ |
Luminosity | 1.732±0.022[3] L☉ |
Surface gravity (log g) | 4.02[7] cgs |
Temperature | 5,890±4.3[8] K |
Metallicity [Fe/H] | +0.12[9] dex |
Rotational velocity (v sin i) | 2[10] km/s |
Age | 4,[9] 5.0–7.9[11] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
ARICNS | data |
Lambda Aurigae, Latinized from λ Aurigae, is the Bayer designation for a solar analog[9] star in the northern constellation of Auriga.[13] It is visible to the naked eye with an apparent visual magnitude of 4.71.[2] Based upon parallax measurements, it is approximately 40.7 light-years (12.5 parsecs) distant from the Earth.[14] The star is drifting further away with a high radial velocity of +66.5 km/s,[1] having come to within 24.4 ly (7.5 pc) some 117,300 years ago.[15] It has a high proper motion, traversing the celestial sphere at the rate of 0.844″ per year.[16]
Properties
This is a G-type main sequence star with a stellar classification of G1 V.[3] It is sometimes listed with a class of G1.5 IV-V Fe-1,[4] which indicates the spectrum is showing some features of a more evolved subgiant star along with a noticeable underabundance of iron. In terms of composition it is similar to the Sun, while the mass and radius are slightly larger.[6] It is 73% more luminous than the Sun[3] and radiates this energy from its outer atmosphere at an effective temperature of 5890 K.[8] At this heat, the star glows with the yellow hue of a G-type star.[17] It has a low level of surface activity and is a candidate Maunder minimum analog.[18]
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.[9] 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.[19]
Name
This star may have been called by the name Al Hurr, meaning the fawn in Arabic.[20] Lambda Aurigae, along with μ Aur and σ Aur, were Kazwini's Al Ḣibāʽ (ألحباع), the Tent.[20] 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 σ Aur as Al Ḣibāʽ III.[21]
In Chinese, 咸池 (Xián Chí), meaning Pool of Harmony, refers to an asterism consisting of λ Aurigae, ρ Aurigae and HD 36041.[22] Consequently, the Chinese name for λ Aurigae itself is 咸池三 (Xián Chí sān, English: the Third Star of Pool of Harmony.)[23]
Observation
From Earth, Lambda Aurigae has an apparent magnitude of 4.71. The closest large neighboring star to Lambda Aurigae is Capella, located 4.5 light-years (1.4 parsecs) away.[24] Hypothetically viewed from Lambda Aurigae, Capella's quadruple star system would have an apparent magnitude of approximately -5.48,[25] about 40 times brighter than Sirius can be seen at maximum brightness from Earth.[26]
References
- ^ a b c d e f g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ 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.
- ^ 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, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101, S2CID 18993744.. See Table 10.
- ^ a b Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
- ^ Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
- ^ 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, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763, S2CID 18775378.
- ^ Chen, Y. Q.; et al. (February 2000), "Chemical composition of 90 F and G disk dwarfs", Astronomy and Astrophysics Supplement, 141 (3): 491–506, arXiv:astro-ph/9912342, Bibcode:2000A&AS..141..491C, doi:10.1051/aas:2000124, S2CID 16273589.
- ^ a b 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, S2CID 18478960.
- ^ a b c d 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, S2CID 17758971.
{{citation}}
: CS1 maint: unflagged free DOI (link) - ^ 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, doi:10.1093/pasj/57.1.13.
- ^ 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, S2CID 27151456.
- ^ "lam Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-19.
{{cite web}}
: CS1 maint: postscript (link) - ^ Kaler, James, "LAMBDA AUR (Lambda Aurigae)", Stars, retrieved 2011-12-11.
- ^ 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, S2CID 18759600. Note: see VizieR catalogue I/311.
- ^ Bailer-Jones, C.A.L.; et al. (2018), "New stellar encounters discovered in the second Gaia data release", Astronomy & Astrophysics, 616: A37, arXiv:1805.07581, Bibcode:2018A&A...616A..37B, doi:10.1051/0004-6361/201833456, S2CID 56269929.
- ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, 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.
- ^ a b Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 91. ISBN 978-0-486-21079-7. Retrieved 2010-12-12.
- ^ 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.
- ^ (in 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.
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日
- ^ "Capella 4". SolStation. Retrieved 10 February 2023.
- ^ "Combined apparent magnitude of 2 stars". WolframΑlpha. Retrieved 10 February 2023.
- ^ "Magnitude Arithmetic". Weekly Topic. Caglow. Archived from the original on 1 February 2012. Retrieved 10 February 2023.