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{{Starbox begin
| name=LBV 1806-20
}}
{{Starbox image
| image=[[File:1806-20 cluster.jpg|280px]]
| caption = 紅外線的[[1806-20星團|星團1806-20]]影像。LBV 1806-20 是在左邊最亮的星。
| credit = [[哈伯太空望遠鏡]]
}}
{{Starbox observe
| epoch=J2000
| ra={{RA|18|08|40.31}}<ref name=figer2005/>
| dec={{DEC|−20|24|41.1}}<ref name=figer2005/>
| constell=[[人馬座]]
}}
{{Starbox character
|type = [[高光度藍變星|LBV]]的候選者<ref name=figer2004/>
|class = O9 - B2<ref name=figer2004/>
|appmag_1_passband=V
|appmag_1=~35<ref name=eikenberry/>
|appmag_2_passband=J
|appmag_2=13.93<ref name=eikenberry/>
|appmag_3_passband=H
|appmag_3=10.75<ref name=eikenberry/>
|appmag_4_passband=K
|appmag_4=8.89<ref name=eikenberry/>
|variable =
}}
{{Starbox astrometry
| radial_v = 
| prop_mo_ra = 
| prop_mo_dec = 
| parallax = 
| p_error = 
| parallax_footnote = 
| dist_ly =
| dist_pc = 8.7k<ref name=bibby/>
| absmag_v = 
| absmag_bol = 
}}
{{Starbox detail
| mass=36<ref name=bibby/>
| radius=46-145{{efn|name=radius}}
| luminosity=~2,000,000<ref name=figer2004/><ref name=naze/><ref name=abdalla/>
| temperature=18,000–32,000<ref name=eikenberry/>
| metal=
| rotation=
| age_myr= 3.0 – 4.5<ref name=figer2005/>
}}
{{starbox catalog
| names = [[2MASS]] J18084031-2024411
}}
{{Starbox reference
| Simbad = NAME+LBV+1806-20
}}
{{Starbox end}}

'''LBV 1806-20'''是[[高光度藍變星]]的候選者，並且可能是一顆[[聯星]]。它與[[太陽]]的距離{{convert|8,700|pc|ly|lk=on|order=flip}}，靠近[[銀心|銀河中心]]。估計它的質量為36[[太陽質量]]，亮度大約是太陽的200萬倍。它雖然有很高的亮度，但因為只有十億分之一的可見光到達地球，因此在[[太陽系]]以可見光看不見這顆恆星。

當首度發現LBV 1806-20時，它被認為是[[恆星光度列表|最亮]]和[[巨大質量恆星列表|已知質量最大]]的恆星，並且挑戰我們對大質量恆星形成的認知。最近的估計認為它離地球稍微近了點；當與聯星結合時，就可能在銀河系中及量恆星的預期參數範圍內。估計它的亮度是太陽的200萬倍，使它成為銀河系中最明亮的恆星之一。

== 位置 ==
LBV 1806-20位於電波[[星雲]]G10.0-03的核心，據信它是由[[恆星風]]提供動力<ref name=yeung/>，是[[疏散星團]][[1806-20星團]]的成員。這個星團是[[銀河系]]最大的[[電離氫區]][[韋斯特豪特31|W31]]的一部分。1806-20星團由一些極不尋常的恆星組成，包括4顆[[沃夫–瑞葉星]]、一些[[OB星]]、和γ射線反覆爆發源[[SGR 1806-20]]（[[磁星]]）<ref name=bibby/>。

== 光譜 ==
LBV 1806-20的光譜類型不確定，可能是可變的。根據氦I的紅外線譜線的[[等效寬度]]，它已被限制在O9和B2之間。光譜顯示出強烈的[[氫原子光譜|氫]]的帕申（Paschen）和布拉開（Brackett）系列，但是也有[[氦]]、鐵II、鎂II、和鈉I的[[譜線|發射線]]。這些譜線都很寬，輪廓不均勻，有些顯現[[天津九|天鵝座P]]的配置<ref name=eikenberry/>。高解析光譜顯示有修譜線是雙重的<ref name=figer2004/>。

== 性質 ==
雖然這顆恆星在2[[微米]]的[[紅外線波長下是顆8[[視星等|等星]]，但根據計算在可見光的波長下只是顆以現在的設備尚無法檢測到的35[[視星等|等星]]。估計在[[銀心|銀河中心]]方向上的塵埃吸收，使它在可見光的星等下降了29星等<ref name=figer2004/>，因此大多數的觀測都是使用[[紅外線]]望遠鏡進行<ref name=bibby/><ref name=figer2005/>。根據其亮度和光譜類型，懷疑它是一顆高光度藍變星。儘管有這樣的懷疑，但由於光度和光譜變化的特徵尚未觀察到，所以它依然只是個候選者<ref name=figer2004/><ref name=naze/>。

== 聯星 ==
為了解是其頻譜中氦I線的雙重性，以及在質量、亮度和年齡估計上的不一致，已經建議LBV 1806-20是聯星。為了解釋其頻譜中雙倍的 HeI 線及其品質、亮度和年齡估計值不一致,LBV 1806-20 已建議為二進位。發射線是單一的，當然就只有一顆恆星，但因為有密集的恆星風，可以預期高光度藍變星可以有雙重的譜線<ref name=figer2004/>。

== 註解 ==
{{notelist|refs=

{{efn | name=radius |利用[[斯特凡-波茲曼定律]]與標稱[[太陽]]的5,772K[[有效溫度]]：
{{clear}}
<math>\sqrt{(5772/18000)^4 * 2,000,000} = 145.42\ R\odot</math>和

<math>\sqrt{(5772/32000)^4 * 2,000,000} = 46.01\ R\odot</math>}}

}}
== 參考資料 ==
{{reflist|refs=

<ref name=figer2004>{{Cite journal | last1 = Figer | first1 = D. F. | last2 = Najarro | first2 = F. | last3 = Kudritzki | first3 = R. P. | doi = 10.1086/423306 | title = The Double-lined Spectrum of LBV 1806-20 | journal = The Astrophysical Journal | volume = 610 | issue = 2 | pages = L109 | year = 2004 | pmid = | pmc = |arxiv = astro-ph/0406316 |bibcode = 2004ApJ...610L.109F }}</ref>

<ref name=naze>{{cite journal|doi=10.1051/0004-6361/201118040|title=The first X-ray survey of Galactic luminous blue variables|journal=Astronomy & Astrophysics|volume=538|pages=A47|year=2012|last1=Nazé|first1=Y.|last2=Rauw|first2=G.|last3=Hutsemékers|first3=D.|bibcode=2012A&A...538A..47N|arxiv = 1111.6375 }}</ref>

<ref name=eikenberry>{{cite journal|doi=10.1086/422180|title=Infrared Observations of the Candidate LBV 1806‐20 and Nearby Cluster Stars|url=https://archive.org/details/sim_astrophysical-journal_2004-11-20_616_1/page/506|journal=The Astrophysical Journal|volume=616|issue=1|pages=506–518|year=2004|last1=Eikenberry|first1=S. S.|last2=Matthews|first2=K.|last3=Lavine|first3=J. L.|last4=Garske|first4=M. A.|last5=Hu|first5=D.|last6=Jackson|first6=M. A.|last7=Patel|first7=S. G.|last8=Barry|first8=D. J.|last9=Colonno|first9=M. R.|last10=Houck|first10=J. R.|last11=Wilson|first11=J. C.|last12=Corbel|first12=S.|last13=Smith|first13=J. D.|bibcode=2004ApJ...616..506E|arxiv = astro-ph/0404435 }}</ref>

<ref name=figer2005>{{cite journal|doi=10.1086/429159|title=Massive Stars in the SGR 1806-20 Cluster|journal=The Astrophysical Journal|volume=622|issue=1|pages=L49|year=2005|last1=Figer|first1=Donald F.|last2=Najarro|first2=Francisco|last3=Geballe|first3=T. R.|last4=Blum|first4=R. D.|last5=Kudritzki|first5=Rolf P.|bibcode=2005ApJ...622L..49F|arxiv = astro-ph/0501560 }}</ref>

<ref name=bibby>{{cite journal|bibcode=2008MNRAS.386L..23B|arxiv=0802.0815|title=A downward revision to the distance of the 1806-20 cluster and associated magnetar from Gemini Near-Infrared Spectroscopy|journal=Monthly Notices of the Royal Astronomical Society: Letters|volume=386|issue=1|pages=L23|author1=Bibby|first1=J. L.|last2=Crowther|first2=P. A.|last3=Furness|first3=J. P.|last4=Clark|first4=J. S.|year=2008|doi=10.1111/j.1745-3933.2008.00453.x}}</ref>

<ref name=yeung>{{cite journal|bibcode=2016ApJ...827...41Y|arxiv=1606.01707|title=Studying the SGR 1806-20/Cl* 1806-20 Region Using the Fermi Large Area Telescope|journal=The Astrophysical Journal|volume=827|issue=1|pages=41|author1=Yeung|first1=Paul K. H.|last2=Kong|first2=Albert K. H.|last3=Tam|first3=P. H. Thomas|last4=Lin|first4=Lupin C. C.|last5=Hui|first5=C. Y.|last6=Hu|first6=Chin-Ping|last7=Cheng|first7=K. S.|year=2016|doi=10.3847/0004-637X/827/1/41}}</ref>

<ref name=abdalla>{{cite journal|doi=10.1051/0004-6361/201628695|title=Extended VHE γ-ray emission towards SGR1806−20, LBV 1806−20, and stellar cluster Cl* 1806−20|journal=Astronomy & Astrophysics|volume=612|pages=A11|year=2018|last1=Abdalla|first1=H.|last2=Abramowski|first2=A.|last3=Aharonian|first3=F.|last4=Ait Benkhali|first4=F.|last5=Akhperjanian|first5=A. G.|last6=Angüner|first6=E. O.|last7=Arrieta|first7=M.|last8=Aubert|first8=P.|last9=Backes|first9=M.|last10=Balzer|first10=A.|last11=Barnard|first11=M.|last12=Becherini|first12=Y.|last13=Becker Tjus|first13=J.|last14=Berge|first14=D.|last15=Bernhard|first15=S.|last16=Bernlöhr|first16=K.|last17=Birsin|first17=E.|last18=Blackwell|first18=R.|last19=Böttcher|first19=M.|last20=Boisson|first20=C.|last21=Bolmont|first21=J.|last22=Bordas|first22=P.|last23=Bregeon|first23=J.|last24=Brun|first24=F.|last25=Brun|first25=P.|last26=Bryan|first26=M.|last27=Bulik|first27=T.|last28=Capasso|first28=M.|last29=Carr|first29=J.|last30=Casanova|first30=S.|displayauthors=29|arxiv=1606.05404}}</ref>

}}

{{Stars of Sagittarius}}

[[Category:高光度藍變星]]
[[Category:人馬座]]
[[Category:超巨星]]
[[Category:2MASS天體]]

LBV 1806-20 - 版本历史

imported>InternetArchiveBot：​Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot

imported>InternetArchiveBot：Add 1 book for verifiability (20251017sim)) #IABot (v2.0.9.5) (GreenC bot