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{{Short description|Star in the constellation Auriga}}
{{Short description|Solar analog star in the constellation Auriga}}
{{Starbox begin
{{Starbox begin
| name = λ Aurigae
| name = λ Aurigae
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| gravity = 4.02<ref name=aaas141_491/>
| gravity = 4.02<ref name=aaas141_491/>
| metal_fe = +0.12<ref name=mnras397_2_757/>
| metal_fe = +0.12<ref name=mnras397_2_757/>
| temperature = {{val|5890|4.3}}<ref name=aaa411_3_559/>
| temperature = {{val|5890|4.3|fmt=commas}}<ref name=aaa411_3_559/>
| luminosity = {{val|1.732|0.022}}<ref name=apj746_1_101/>
| luminosity = {{val|1.732|0.022}}<ref name=apj746_1_101/>
| rotational_velocity = 2<ref name=pasj57_1_13/>
| rotational_velocity = 2<ref name=pasj57_1_13/>
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{{Starbox end}}
{{Starbox end}}


'''Lambda Aurigae''', [[Romanization of Greek|Latinized]] from λ Aurigae, is the [[Bayer designation]] for a [[solar analog]]<ref name=mnras397_2_757/> [[star]] in the northern [[constellation]] of [[Auriga (constellation)|Auriga]].<ref name=kaler/> It is visible to the naked eye with an [[apparent visual magnitude]] of 4.71.<ref name=clpl4_99/> Based upon [[parallax]] measurements, it is approximately {{Convert|40.7|ly|pc|abbr=off|lk=on}} distant from the Earth.<ref name=aaa474_2_653/> The star is drifting further away with a high [[radial velocity]] of +66.5&nbsp;km/s,<ref name=GaiaDR2/> having come to within {{convert|7.4945|pc|ly|1|adj=ri1|order=flip|abbr=on}} some 117,300&nbsp;years ago.<ref name=Bailer_et_al_2018/>
'''Lambda Aurigae''', [[Romanization of Greek|Latinized]] from λ Aurigae, is the [[Bayer designation]] for a [[solar analog]]<ref name=mnras397_2_757/> [[star]] in the northern [[constellation]] of [[Auriga (constellation)|Auriga]].<ref name=kaler/> It is visible to the naked eye with an [[apparent visual magnitude]] of 4.71.<ref name=clpl4_99/> Based upon [[parallax]] measurements, it is approximately {{Convert|40.7|ly|pc|abbr=off|lk=on}} distant from the Earth.<ref name=aaa474_2_653/> The star is drifting further away with a high [[radial velocity]] of +66.5&nbsp;km/s,<ref name=GaiaDR2/> having come to within {{convert|7.4945|pc|ly|1|adj=ri1|order=flip|abbr=on}} some 117,300&nbsp;years ago.<ref name=Bailer_et_al_2018/> It has a high [[proper motion]], traversing the [[celestial sphere]] at the rate of {{Val|0.844|ul=arcsecond}} per year.<ref name=Lepine2005/>


==Properties==
==Properties==
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==Name==
==Name==
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 [[Rho Aurigae|ρ 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/>
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/>


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>

==Observation==
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>


==References==
==References==
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| journal=Astronomy and Astrophysics
| journal=Astronomy and Astrophysics
| doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H
| doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H
| arxiv=0811.3982 | postscript=. }}</ref>
| arxiv=0811.3982 | s2cid=118577511 | postscript=. }}</ref>


<ref name=aaa474_2_653>{{citation | first1=Floor | last1=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | arxiv=0708.1752v1 | doi=10.1051/0004-6361:20078357 | journal=[[Astronomy and Astrophysics]] | postscript=. }} ''Note:'' see VizieR catalogue [http://vizier.u-strasbg.fr/viz-bin/Cat?I/311 I/311].</ref>
<ref name=aaa474_2_653>{{citation | first1=Floor | last1=van Leeuwen |date=November 2007 | title=Validation of the new Hipparcos reduction | volume=474 | issue=2 | pages=653–664 | bibcode=2007A&A...474..653V | arxiv=0708.1752v1 | doi=10.1051/0004-6361:20078357 | journal=[[Astronomy and Astrophysics]] | s2cid=18759600 | postscript=. }} ''Note:'' see VizieR catalogue [http://vizier.u-strasbg.fr/viz-bin/Cat?I/311 I/311].</ref>


<ref name=aaa411_3_559>{{citation | display-authors=1 | last1=Kovtyukh | first1=V. V. | last2=Soubiran | first2=C. | last3=Belik | first3=S. I. | last4=Gorlova | first4=N. I. | title=High precision effective temperatures for 181 F-K dwarfs from line-depth ratios | journal=[[Astronomy and Astrophysics]] | volume=411 | issue=3 | pages=559–564 | date=2003 | doi=10.1051/0004-6361:20031378 | bibcode=2003A&A...411..559K | arxiv=astro-ph/0308429 | postscript=. }}</ref>
<ref name=aaa411_3_559>{{citation | display-authors=1 | last1=Kovtyukh | first1=V. V. | last2=Soubiran | first2=C. | last3=Belik | first3=S. I. | last4=Gorlova | first4=N. I. | title=High precision effective temperatures for 181 F-K dwarfs from line-depth ratios | journal=[[Astronomy and Astrophysics]] | volume=411 | issue=3 | pages=559–564 | date=2003 | doi=10.1051/0004-6361:20031378 | bibcode=2003A&A...411..559K | arxiv=astro-ph/0308429 | s2cid=18478960 | postscript=. }}</ref>


<ref name=apj687_2_1264>{{citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 |date=November 2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M | arxiv=0807.1686 | postscript=. }}</ref>
<ref name=apj687_2_1264>{{citation | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 |date=November 2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M | arxiv=0807.1686 | s2cid=27151456 | postscript=. }}</ref>


<ref name=aaas141_491>{{citation | display-authors=1 | last1=Chen | first1=Y. Q. | last2=Nissen | first2=P. E. | last3=Zhao | first3=G. | last4=Zhang | first4=H. W. | last5=Benoni | first5=T. | title=Chemical composition of 90 F and G disk dwarfs | journal=Astronomy and Astrophysics Supplement | volume=141 | issue=3 | pages=491–506 |date=February 2000 | doi=10.1051/aas:2000124 | bibcode=2000A&AS..141..491C | arxiv=astro-ph/9912342 | postscript=. }}</ref>
<ref name=aaas141_491>{{citation | display-authors=1 | last1=Chen | first1=Y. Q. | last2=Nissen | first2=P. E. | last3=Zhao | first3=G. | last4=Zhang | first4=H. W. | last5=Benoni | first5=T. | title=Chemical composition of 90 F and G disk dwarfs | journal=Astronomy and Astrophysics Supplement | volume=141 | issue=3 | pages=491–506 |date=February 2000 | doi=10.1051/aas:2000124 | bibcode=2000A&AS..141..491C | arxiv=astro-ph/9912342 | s2cid=16273589 | postscript=. }}</ref>


<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | pages=99 | date=1966 | bibcode=1966CoLPL...4...99J | postscript=. }}</ref>
<ref name=clpl4_99>{{citation | display-authors=1 | last1=Johnson | first1=H. L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R. I. | last4=Wisniewskj | first4=W. Z. | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | pages=99 | date=1966 | bibcode=1966CoLPL...4...99J | postscript=. }}</ref>
Line 98: Line 101:
<ref name=aaa68_1_27>{{citation | last1=Kovacs | first1=N. | last2=Foy | first2=R. | title=A detailed analysis of three stars in the Eggen's Epsilon INDI moving group | journal=Astronomy and Astrophysics | volume=68 | issue=1–2 | pages=27–31 |date=August 1978 | bibcode=1978A&A....68...27K | postscript=. }}</ref>
<ref name=aaa68_1_27>{{citation | last1=Kovacs | first1=N. | last2=Foy | first2=R. | title=A detailed analysis of three stars in the Eggen's Epsilon INDI moving group | journal=Astronomy and Astrophysics | volume=68 | issue=1–2 | pages=27–31 |date=August 1978 | bibcode=1978A&A....68...27K | postscript=. }}</ref>


<ref name=apjss168_2_297>{{citation | display-authors=1 | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6=Jeff A. | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | journal=The Astrophysical Journal Supplement Series | volume=168 | issue=2 | pages=297–318 |date=February 2007 | doi=10.1086/509763 | bibcode=2007ApJS..168..297T | arxiv=astro-ph/0607235 | postscript=. }}</ref>
<ref name=apjss168_2_297>{{citation | display-authors=1 | last1=Takeda | first1=Genya | last2=Ford | first2=Eric B. | last3=Sills | first3=Alison | last4=Rasio | first4=Frederic A. | last5=Fischer | first5=Debra A. | last6=Valenti | first6=Jeff A. | title=Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog | journal=The Astrophysical Journal Supplement Series | volume=168 | issue=2 | pages=297–318 |date=February 2007 | doi=10.1086/509763 | bibcode=2007ApJS..168..297T | arxiv=astro-ph/0607235 | s2cid=18775378 | postscript=. }}</ref>


<ref name=apj746_1_101>{{citation | display-authors=1 | last1=Boyajian | first1=Tabetha S. | last2=McAlister | first2=Harold A. | last3=van Belle | first3=Gerard | last4=Gies | first4=Douglas R. | last5=ten Brummelaar | first5=Theo A. | last6=von Braun | first6=Kaspar | last7=Farrington | first7=Chris | last8=Goldfinger | first8=P. J. | last9=O'Brien | first9=David | last10=Parks | first10=J. Robert | last11=Richardson | first11=Noel D. | last12=Ridgway | first12=Stephen | last13=Schaefer | first13=Gail | last14=Sturmann | first14=Laszlo | last15=Sturmann | first15=Judit | last16=Touhami | first16=Yamina | last17=Turner | first17=Nils H. | last18=White | first18=Russel | title=Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars | journal=The Astrophysical Journal | volume=746 | issue=1 | page=101 |date=February 2012 | doi=10.1088/0004-637X/746/1/101 | bibcode=2012ApJ...746..101B | arxiv=1112.3316 | postscript=. }}. See Table 10.</ref>
<ref name=apj746_1_101>{{citation | display-authors=1 | last1=Boyajian | first1=Tabetha S. | last2=McAlister | first2=Harold A. | last3=van Belle | first3=Gerard | last4=Gies | first4=Douglas R. | last5=ten Brummelaar | first5=Theo A. | last6=von Braun | first6=Kaspar | last7=Farrington | first7=Chris | last8=Goldfinger | first8=P. J. | last9=O'Brien | first9=David | last10=Parks | first10=J. Robert | last11=Richardson | first11=Noel D. | last12=Ridgway | first12=Stephen | last13=Schaefer | first13=Gail | last14=Sturmann | first14=Laszlo | last15=Sturmann | first15=Judit | last16=Touhami | first16=Yamina | last17=Turner | first17=Nils H. | last18=White | first18=Russel | title=Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars | journal=The Astrophysical Journal | volume=746 | issue=1 | page=101 |date=February 2012 | doi=10.1088/0004-637X/746/1/101 | bibcode=2012ApJ...746..101B | arxiv=1112.3316 | s2cid=18993744 | postscript=. }}. See Table 10.</ref>


<ref name=SIMBAD>{{cite simbad | title=lam Aur | access-date=2012-08-19 | postscript=. }}</ref>
<ref name=SIMBAD>{{cite simbad | title=lam Aur | access-date=2012-08-19 | postscript=. }}</ref>


<ref name=kaler>{{citation | first1=James | last=Kaler | title=LAMBDA AUR (Lambda Aurigae) | work=Stars | url=http://stars.astro.illinois.edu/sow/lambdaaur.html | accessdate=2011-12-11 | postscript=. }}</ref>
<ref name=kaler>{{citation | first1=James | last1=Kaler | title=LAMBDA AUR (Lambda Aurigae) | work=Stars | url=http://stars.astro.illinois.edu/sow/lambdaaur.html | accessdate=2011-12-11 | postscript=. }}</ref>


<ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |accessdate=2012-01-16 |postscript=. |url-status=dead |archiveurl=https://www.webcitation.org/6630AbtJZ?url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archivedate=March 10, 2012 }}</ref>
<ref name=csiro>{{citation|title=The Colour of Stars |date=December 21, 2004 |work=Australia Telescope, Outreach and Education |publisher=[[Commonwealth Scientific and Industrial Research Organisation]] |url=http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |accessdate=2012-01-16 |postscript=. |url-status=dead |archiveurl=https://web.archive.org/web/20120318151427/http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html |archivedate=March 18, 2012 }}</ref>


<ref name=mnras397_2_757>{{citation | last1=Greaves | first1=J. S. | last2=Wyatt | first2=M. C. | last3=Bryden | first3=G. | title=Debris discs around nearby solar analogues | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=397 | issue=2 | pages=757–762 |date=August 2009 | doi=10.1111/j.1365-2966.2009.15048.x | bibcode=2009MNRAS.397..757G | arxiv=0907.3677 | postscript=. }}</ref>
<ref name=mnras397_2_757>{{citation | last1=Greaves | first1=J. S. | last2=Wyatt | first2=M. C. | last3=Bryden | first3=G. | title=Debris discs around nearby solar analogues | journal=[[Monthly Notices of the Royal Astronomical Society]] | volume=397 | issue=2 | pages=757–762 |date=August 2009 | doi=10.1111/j.1365-2966.2009.15048.x | bibcode=2009MNRAS.397..757G | arxiv=0907.3677 | s2cid=17758971 | postscript=. }}</ref>


<ref name=rhoads1971>{{citation | first1=Jack W. | last1=Rhoads | title=Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars | publisher=[[Jet Propulsion Laboratory]] | location=California Institute of Technology | date=November 15, 1971 | url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19720005197_1972005197.pdf | accessdate=2012-08-19 | postscript=. }}</ref>
<ref name=rhoads1971>{{citation | first1=Jack W. | last1=Rhoads | title=Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars | publisher=[[Jet Propulsion Laboratory]] | location=California Institute of Technology | date=November 15, 1971 | url=https://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19720005197_1972005197.pdf | accessdate=2012-08-19 | postscript=. }}</ref>
Line 138: Line 141:
| volume=616 | pages=A37 | date=2018
| volume=616 | pages=A37 | date=2018
| arxiv=1805.07581 | bibcode=2018A&A...616A..37B
| arxiv=1805.07581 | bibcode=2018A&A...616A..37B
| doi=10.1051/0004-6361/201833456 | postscript=. }}</ref>
| doi=10.1051/0004-6361/201833456 | s2cid=56269929 | postscript=. }}</ref>


<ref name=Keenan_McNeil_1989>{{citation
<ref name=Keenan_McNeil_1989>{{citation
Line 146: Line 149:
| volume=71 | pages=245 | year=1989 | postscript=.
| volume=71 | pages=245 | year=1989 | postscript=.
| bibcode=1989ApJS...71..245K | doi=10.1086/191373 }}</ref>
| bibcode=1989ApJS...71..245K | doi=10.1086/191373 }}</ref>

<ref name=Lepine2005>{{citation
| last1=Lépine | first1=Sébastien | last2=Shara | first2=Michael M.
| title=A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)
| journal=The Astronomical Journal
| volume=129 | issue=3 | pages=1483–1522 | date=March 2005
| doi=10.1086/427854 | bibcode=2005AJ....129.1483L
| arxiv=astro-ph/0412070 | s2cid=2603568 | postscript=. }}</ref>

<ref name="SolStation">{{cite web | url=http://www.solstation.com/stars2/capella4.htm|title = Capella 4 | publisher = SolStation
| access-date = 10 February 2023}}</ref>

<ref name="Wolfram">{{cite web | url=https://www.wolframalpha.com/widgets/view.jsp?id=aa35819112b597d719cc24ba31e63c34|title = Combined apparent magnitude of 2 stars | publisher = WolframΑlpha
| access-date = 10 February 2023}}</ref>


}}
}}
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[[Category:G-type subgiants]]
[[Category:G-type subgiants]]
[[Category:Solar-type stars|Aurigae, Lambda]]
[[Category:Solar-type stars|Aurigae, Lambda]]
[[Category:Maunder Minimum]]
<!-- Other -->
<!-- Other -->
[[Category:Auriga (constellation)]]
[[Category:Auriga (constellation)]]
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[[Category:Henry Draper Catalogue objects|034411]]
[[Category:Henry Draper Catalogue objects|034411]]
[[Category:Hipparcos objects|024813]]
[[Category:Hipparcos objects|024813]]
[[Category:HR objects|1729]]
[[Category:Bright Star Catalogue objects|1729]]

Revision as of 14:25, 20 August 2023

λ Aurigae
Location of λ Aurigae (circled)
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]
Distance40.7 ± 0.1 ly
(12.48 ± 0.03 pc)
Absolute magnitude (MV)4.20[5]
Details
Mass1.081+0.054
−0.029[6] M☉
Radius1.331±0.021[3] R☉
Luminosity1.732±0.022[3] L☉
Surface gravity (log g)4.02[7] cgs
Temperature5,890±4.3[8] K
Metallicity [Fe/H]+0.12[9] dex
Rotational velocity (v sin i)2[10] km/s
Age4,[9] 5.0–7.9[11] Gyr
Other designations
λ Aur, 15 Aurigae, BD+39° 1248, FK5 1145, GJ 197, HD 34411, HIP 24813, HR 1729, SAO 40233, LFT 403, LHS 1753, LTT 11625[12]
Database references
SIMBADdata
ARICNSdata

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

  1. ^ 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.
  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): 99, Bibcode:1966CoLPL...4...99J.
  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, arXiv:1112.3316, Bibcode:2012ApJ...746..101B, doi:10.1088/0004-637X/746/1/101, S2CID 18993744.. See Table 10.
  4. ^ 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.
  5. ^ 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.
  6. ^ 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.
  7. ^ 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.
  8. ^ 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.
  9. ^ 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)
  10. ^ 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.
  11. ^ 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.
  12. ^ "lam Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-19.{{cite web}}: CS1 maint: postscript (link)
  13. ^ Kaler, James, "LAMBDA AUR (Lambda Aurigae)", Stars, retrieved 2011-12-11.
  14. ^ 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.
  15. ^ 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.
  16. ^ 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.
  17. ^ "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.
  18. ^ 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.
  19. ^ 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.
  20. ^ 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.
  21. ^ 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.
  22. ^ (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.
  23. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 13 日
  24. ^ "Capella 4". SolStation. Retrieved 10 February 2023.
  25. ^ "Combined apparent magnitude of 2 stars". WolframΑlpha. Retrieved 10 February 2023.
  26. ^ "Magnitude Arithmetic". Weekly Topic. Caglow. Archived from the original on 1 February 2012. Retrieved 10 February 2023.
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