Lambda Aurigae: Difference between revisions
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{{Short description|Solar analog star in the constellation Auriga}} |
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{{Starbox begin |
{{Starbox begin |
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| name = |
| name = λ Aurigae |
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}} |
}} |
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{{Starbox image |
{{Starbox image |
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| image |
| image= |
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{{Location mark |
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<div style="position: relative">[[File:Auriga IAU.svg|250px|alt=Diagram showing star positions and boundaries of the Auriga constellation and its surroundings]] |
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|image=Auriga constellation map.svg|alt=|float=center|width=260 |
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<div style="position: absolute; left: 56.6%; top: 39.2%">[[File:Cercle rouge 100%.svg|12px]]</div> |
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|label=|position=right |
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</div> |
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|mark=Red circle.svg|mark_width=8|mark_link=λ Aurigae |
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⚫ | |||
|x=590|y=443 |
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}} |
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⚫ | |||
}} |
}} |
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{{Starbox observe |
{{Starbox observe |
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| epoch = J2000 |
| epoch = J2000 |
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| constell = [[Auriga (constellation)|Auriga]] |
| constell = [[Auriga (constellation)|Auriga]] |
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| ra = {{RA|05|19|08. |
| ra = {{RA|05|19|08.47546}}<ref name=GaiaDR2/> |
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| dec = {{DEC|+40|05|56. |
| dec = {{DEC|+40|05|56.5896}}<ref name=GaiaDR2/> |
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| appmag_v = 4.71<ref name=clpl4_99/> |
| appmag_v = 4.71<ref name=clpl4_99/> |
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}} |
}} |
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{{Starbox character |
{{Starbox character |
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| class = G1 V<ref name=apj746_1_101/> |
| class = G1 V<ref name=apj746_1_101/> or {{nowrap|G1.5 IV-V Fe-1}}<ref name=Keenan_McNeil_1989/> |
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| r-i = 0.32 |
| r-i = 0.32 |
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| v-r = |
| v-r = |
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}} |
}} |
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{{Starbox astrometry |
{{Starbox astrometry |
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| radial_v = 66. |
| radial_v = {{val|+66.53|0.14}}<ref name=GaiaDR2/> |
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| prop_mo_ra = + |
| prop_mo_ra = +520.581<ref name=GaiaDR2/> |
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| prop_mo_dec = |
| prop_mo_dec = −664.826<ref name=GaiaDR2/> |
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| parallax = |
| parallax = 80.1054 |
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| p_error = 0. |
| p_error = 0.2158 |
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| parallax_footnote = <ref name= |
| parallax_footnote = <ref name=GaiaDR2/> |
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| absmag_v = |
| absmag_v = 4.20<ref name=Holmberg2009/> |
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}} |
}} |
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{{Starbox detail |
{{Starbox detail |
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| radius = {{val|1.331|0.021}}<ref name=apj746_1_101/> |
| radius = {{val|1.331|0.021}}<ref name=apj746_1_101/> |
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| gravity = 4.02<ref name=aaas141_491/> |
| gravity = 4.02<ref name=aaas141_491/> |
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| metal_fe = +0. |
| metal_fe = +0.12<ref name=mnras397_2_757/> |
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| temperature = {{val|5890|4.3}}<ref name=aaa411_3_559/> |
| temperature = {{val|5890|4.3|fmt=commas}}<ref name=aaa411_3_559/> |
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| luminosity = {{val|1.732|0.022}}<ref name=apj746_1_101/> |
| luminosity = {{val|1.732|0.022}}<ref name=apj746_1_101/> |
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| rotational_velocity = 2<ref name=pasj57_1_13/> |
| rotational_velocity = 2<ref name=pasj57_1_13/> |
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| age_gyr = 5.0–7.9<ref name=apj687_2_1264/> |
| age_gyr = 4,<ref name=mnras397_2_757/> 5.0–7.9<ref name=apj687_2_1264/> |
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}} |
}} |
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{{Starbox catalog |
{{Starbox catalog |
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| names = |
| names = {{odlist | B=λ Aur | F=15 Aurigae | BD=+39° 1248 | FK5=1145 | GJ=197 | HD=34411 | HIP=24813 | HR=1729 | LFT=403 | LHS=1753 | LTT=11625 | SAO=40233 }}<ref name=SIMBAD/> |
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}} |
}} |
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{{Starbox reference |
{{Starbox reference |
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|Simbad=lam+Aur |
| Simbad=lam+Aur |
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|ARICNS=00434 |
| ARICNS=00434 |
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}} |
}} |
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{{Starbox end}} |
{{Starbox end}} |
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⚫ | '''Lambda Aurigae''' |
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⚫ | '''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 km/s,<ref name=GaiaDR2/> having come to within {{convert|7.4945|pc|ly|1|adj=ri1|order=flip|abbr=on}} some 117,300 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/> |
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⚫ | This is a [[G-type main sequence star]] with a [[stellar classification]] of G1 V.<ref name=apj746_1_101/> In terms of composition it is similar to the [[Sun]], while the mass and radius are slightly larger.<ref name=apjss168_2_297/> It is 73% more luminous than the Sun<ref name=apj746_1_101/> and radiates this energy from its [[stellar atmosphere|outer atmosphere]] at an [[effective temperature]] of {{val|5890|u=K}}.<ref name=aaa411_3_559/> At this heat, the star glows with the yellow hue of a [[G-type star]].<ref name=csiro/> It has a low level of surface activity and is a candidate [[Maunder minimum]] analog.<ref name="MPB32_2_27"/> |
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==Properties== |
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⚫ | Lambda Aurigae has been examined for the presence of excess infrared emission that may indicate the presence of a circumstellar [[debris disk|disk of dust]], but no significant surplus has been observed.<ref name=mnras397_2_757/> It is a possible member of the [[Epsilon Indi |
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⚫ | This is a [[G-type main sequence star]] with a [[stellar classification]] of G1 V.<ref name=apj746_1_101/> It is sometimes listed with a class of G1.5 IV-V Fe-1,<ref name=Keenan_McNeil_1989/> which indicates the [[stellar spectrum|spectrum]] is showing some features of a more [[stellar evolution|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.<ref name=apjss168_2_297/> It is 73% more luminous than the Sun<ref name=apj746_1_101/> and radiates this energy from its [[stellar atmosphere|outer atmosphere]] at an [[effective temperature]] of {{val|5890|u=K}}.<ref name=aaa411_3_559/> At this heat, the star glows with the yellow hue of a [[G-type star]].<ref name=csiro/> It has a low level of surface activity and is a candidate [[Maunder minimum]] analog.<ref name="MPB32_2_27"/> |
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⚫ | Lambda Aurigae has been examined for the presence of excess infrared emission that may indicate the presence of a circumstellar [[debris disk|disk of dust]], but no significant surplus has been observed.<ref name=mnras397_2_757/> It is a possible member of the [[Epsilon Indi Moving Group]] of stars that share a [[common proper motion|common motion]] through space. The [[space velocity (astronomy)|space velocity]] components of this star are {{nowrap|[U, V, W]}} = {{nowrap|[+76, –39, –6] km/s}}.<ref name=aaa68_1_27/> |
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==Name== |
==Name== |
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This star |
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 |
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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{{reflist|refs= |
{{reflist|refs= |
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<ref name=GaiaDR2>{{Cite Gaia DR2|188771135583573504}}</ref> |
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<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> |
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<ref name=Holmberg2009>{{citation |
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<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> |
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| display-authors=1 | last1=Holmberg | first1=J. |
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| last2=Nordström | first2=B. | last3=Andersen | first3=J. |
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| title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics |
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| volume=501 | issue=3 |date=July 2009 | pages=941–947 |
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| journal=Astronomy and Astrophysics |
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| doi=10.1051/0004-6361/200811191 | bibcode=2009A&A...501..941H |
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| arxiv=0811.3982 | s2cid=118577511 | postscript=. }}</ref> |
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<ref name= |
<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> |
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<ref name= |
<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> |
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<ref name= |
<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> |
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<ref name= |
<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> |
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<ref name= |
<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> |
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<ref name=pasj57_1_13>{{citation | display-authors=1 | last1=Takeda | first1=Yoichi | last2=Sato | first2=Bun'ei | last3=Kambe | first3=Eiji | last4=Masuda | first4=Seiji | last5=Izumiura | first5=Hideyuki | last6=Watanabe | first6=Etsuji | last7=Ohkubo | first7=Michiko | last8=Yanagisawa | first8=Kenshi | last9=Yasaka | first9=Yoshiro | title=High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards | journal=Publications of the Astronomical Society of Japan | volume=57 | issue=1 | pages=13–25 |date=February 2005 | bibcode=2005PASJ...57...13T | postscript=. | doi=10.1093/pasj/57.1.13| doi-access=free }}</ref> |
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⚫ | <ref name=allen1962>{{cite book | last=Allen | first=R. H. | date=1963 | authorlink=Richard Hinckley Allen | title=Star Names: Their Lore and Meaning | url= |
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⚫ | <ref name=allen1962>{{cite book | last=Allen | first=R. H. | date=1963 | authorlink=Richard Hinckley Allen | title=Star Names: Their Lore and Meaning | url=https://archive.org/details/starnamestheirlo00alle/page/91 | accessdate=2010-12-12 | edition=Reprint | publisher=Dover Publications Inc | location=New York, NY | isbn=978-0-486-21079-7 | page=[https://archive.org/details/starnamestheirlo00alle/page/91 91] | url-access=registration }}</ref> |
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<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> |
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<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> |
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<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> |
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<ref name=SIMBAD>{{ |
<ref name=SIMBAD>{{cite simbad | title=lam Aur | access-date=2012-08-19 | postscript=. }}</ref> |
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<ref name=kaler>{{citation | first1=James | |
<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> |
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<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=. | |
<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> |
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<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> |
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<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 | |
<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> |
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<ref name="MPB32_2_27">{{citation |
<ref name="MPB32_2_27">{{citation |
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| bibcode = 2012ApJ...747L..32L |
| bibcode = 2012ApJ...747L..32L |
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| postscript = . |
| postscript = . |
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| doi-access= free |
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}}</ref> |
}}</ref> |
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<ref name=Bailer_et_al_2018>{{citation |
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| title=New stellar encounters discovered in the second Gaia data release |
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| last1=Bailer-Jones | first1=C.A.L. | last2=Rybizki | first2=J. |
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| last3=Andrae | first3=R. | last4=Fouesnea | first4=M. |
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| display-authors=1 | journal=Astronomy & Astrophysics |
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| volume=616 | pages=A37 | date=2018 |
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| arxiv=1805.07581 | bibcode=2018A&A...616A..37B |
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| doi=10.1051/0004-6361/201833456 | s2cid=56269929 | postscript=. }}</ref> |
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<ref name=Keenan_McNeil_1989>{{citation |
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| title=The Perkins catalog of revised MK types for the cooler stars |
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| last1=Keenan | first1=Philip C. | last2=McNeil | first2=Raymond C. |
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| journal=Astrophysical Journal Supplement Series |
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| volume=71 | pages=245 | year=1989 | postscript=. |
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| bibcode=1989ApJS...71..245K | doi=10.1086/191373 }}</ref> |
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<ref name=Lepine2005>{{citation |
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| last1=Lépine | first1=Sébastien | last2=Shara | first2=Michael M. |
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| title=A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog) |
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| journal=The Astronomical Journal |
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| volume=129 | issue=3 | pages=1483–1522 | date=March 2005 |
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| doi=10.1086/427854 | bibcode=2005AJ....129.1483L |
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| 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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}} |
}} |
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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.