编辑“︁WOH G64”︁

{{Starbox begin 
| name=WOH G64
}}
{{Starbox image
 | image=
[[File:WOH G64 VLTI.jpg|300 px]]
|caption=[[甚大望遠鏡|VLTI]]恆星周圍塵埃環的影像。
|credit=ESO
}}
{{Starbox observe
| epoch=[[J2000.0]]
| ra={{RA|04|55|10.5252}}<ref name=dr2/>
| dec={{DEC|−68|20|29.998}}<ref name=dr2/>
| appmag_v=17.7 - 18.8<ref name=bhardwai2019>{{cite journal |bibcode=2019ApJ...884...20B |title=Multiwavelength Period-Luminosity and Period-Luminosity-Color Relations at Maximum Light for Mira Variables in the Magellanic Clouds |last1=Bhardwaj |first1=Anupam |last2=Kanbur |first2=Shashi |last3=He |first3=Shiyuan |last4=Rejkuba |first4=Marina |last5=Matsunaga |first5=Noriyuki |last6=De Grijs |first6=Richard |last7=Sharma |first7=Kaushal |last8=Singh |first8=Harinder P. |last9=Baug |first9=Tapas |last10=Ngeow |first10=Chow-Choong |last11=Ou |first11=Jia-Yu |journal=The Astrophysical Journal |year=2019 |volume=884 |issue=1 |page=20 |doi=10.3847/1538-4357/ab38c2 |arxiv=1908.01795 |s2cid=199452754 |doi-access=free }}</ref>
| constell= [[劍魚座]]（[[大麥哲倫星系|LMC]]）
}}
{{Starbox character
| type = [[OH/IR star|OH/IR]] [[紅超巨星]]
| class=M5 I<ref name=levesque>{{Cite journal | last1 = Levesque | first1 = E. M. | last2 = Massey | first2 = P. | last3 = Plez | first3 = B. | last4 = Olsen | first4 = K. A. G. | title = The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known? | doi = 10.1088/0004-6256/137/6/4744 | journal = The Astronomical Journal | volume = 137 | issue = 6 | pages = 4744 | year = 2009 |arxiv = 0903.2260 |bibcode = 2009AJ....137.4744L | s2cid = 18074349 }}</ref>– M7.5e<ref name=vanloon/><ref name=elias/>
| appmag_1_passband=K
| appmag_1=6.849<ref name=2mass/>
| appmag_2_passband=R
| appmag_2=15.69<ref name=macho/>
| appmag_3_passband=G
| appmag_3=15.0971<ref name=dr2/>
| appmag_4_passband=I
| appmag_4=12.795<ref name=ogle/>
| appmag_5_passband=J
| appmag_5=9.252<ref name=2mass/>
| appmag_6_passband=H
| appmag_6=7.745<ref name=2mass/>
| b-v=
| u-b=
| variable=富碳[[長週期變星|LPV]]（[[米拉變星|米拉]]？）<ref name=ogle/>
}}
{{Starbox astrometry
| radial_v={{val|294|2}}<ref name=levesque/>
| prop_mo_ra=1.108<ref name=dr2/>
| prop_mo_dec=−1.348<ref name=dr2/>
| parallax=−0.2280
| p_error=0.0625
| parallax_footnote = <ref name=dr2/>
| dist_ly=160,000
| dist_pc=50,000<ref name=levesque/>
| absmag_v = −6.00<ref name=levesque/>
}}
{{Starbox detail
| mass={{val|25|5|fmt=commas}} (''initial mass'')<ref name=levesque/>
| radius={{val|1,540|77|fmt=commas}}<ref name=levesque/><ref name=RSGLevesque>{{Cite conference|last=Levesque|first=E. M.|date=June 2010|title=The Physical Properties of Red Supergiants|conference=Hot and Cool: Bridging Gaps in Massive Star Evolution ASP Conference Series|volume=425|pages=103|url=https://articles.adsabs.harvard.edu/pdf/2010ASPC..425..103L|bibcode=2010ASPC..425..103L|arxiv=0911.4720|s2cid=8921166|access-date=2024-11-27|archive-date=2024-12-03|archive-url=https://web.archive.org/web/20241203002844/https://articles.adsabs.harvard.edu/pdf/2010ASPC..425..103L|dead-url=no}}</ref><ref name=Beasor2022>{{Cite journal |last1=Beasor |first1=Emma R. |last2=Smith |first2=Nathan |date=2022-05-01 |title=The Extreme Scarcity of Dust-enshrouded Red Supergiants: Consequences for Producing Stripped Stars via Winds |journal=The Astrophysical Journal |volume=933 |issue=1 |page=41 |doi=10.3847/1538-4357/ac6dcf |arxiv=2205.02207 |bibcode=2022ApJ...933...41B |s2cid=248512934 |doi-access=free}}</ref>
| luminosity={{val|282,000|34,400|30,700|fmt=commas}}<ref name=levesque/>
| temperature={{val|3,400|25|fmt=commas}}<ref name=levesque/>
| metal=
| rotation=
| gravity=+0.0<ref name="Groenewegen2018">{{Cite journal|last1=Groenewegen|first1=Martin A. T.|last2=Sloan|first2=Greg C.|date=2018|title=Luminosities and mass-loss rates of Local Group AGB stars and Red Supergiants|journal=[[Astronomy & Astrophysics]]|volume=609|pages=A114|doi=10.1051/0004-6361/201731089|arxiv=1711.07803|bibcode=2018A&A...609A.114G|s2cid=59327105|issn=0004-6361}}</ref>–−0.5<ref name=levesque/>
| age_myr=≤5<ref name=davies2018>{{cite journal |arxiv=1804.06417 |doi=10.1093/mnras/sty1302 |title=The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys–Davidson limit revisited |year=2018 |last1=Davies |first1=Ben |last2=Crowther |first2=Paul A. |last3=Beasor |first3=Emma R. |s2cid=59459492 |journal=Monthly Notices of the Royal Astronomical Society |volume=478 |issue=3 |pages=3138–3148 |doi-access=free |bibcode=2018MNRAS.478.3138D }}</ref>
}}
{{Starbox catalog
| names=WOH&nbsp;G064, [[2MASS]]&nbsp;J04551048-6820298, [[IRAS]]&nbsp;04553-6825, MSX LMC 1182
}}
{{Starbox reference
| Simbad=WOH+G+64
}}
{{Starbox end}}

'''WOH G64'''（'''IRAS 04553-6825'''）是位於南天[[星座]][[劍魚座]]的[[銀河系]]衛星星系，[[大麥哲倫星系]]（LMC）中，一顆不尋常的<ref name=levesque/>[[紅超巨星]]。它是具有明確半徑的[[巨大恆星列表|已知最大恆星]]<ref name=levesque/><ref name="SAGE">{{cite journal |last1=Jones |first1=Olivia |last2=Woods |first2=Paul |last3=Kemper |first3=Franziska |last4=Kraemer |first4=Elena |last5=Sloan |first5=G. |last6=Srinivasan |first6=Sivakrishnan |last7=Oliveira |first7=Joana |last8=van Loon |first8=Jacco |last9=Boyer |first9=Martha |last10=Sargent |first10=Benjamin |last11=Mc Donald |first11=I. |last12=Meixner |first12=Margaret |last13=Zijlstra |first13=A. |last14=Ruffel |first14=Paul |last15=Lagadec |first15=Eric |last16=Pauly |first16=Tyler |title=The SAGE-Spec Spitzer Legacy program: the life-cycle of dust and gas in the Large Magellanic Cloud. Point source classification – III |journal=Monthly Notices of the Royal Astronomical Society |date=May 7, 2017 |volume=470 |issue=3 |pages=3250–3282 |doi=10.1093/mnras/stx1101 |url=https://www.researchgate.net/publication/316780448 |access-date=23 June 2022|doi-access=free |arxiv=1705.02709 }}</ref>。它是[[恆星光度列表|最亮]]和[[巨大質量恆星列表|最大質量]]的[[紅超巨星]]之一，其半徑約為[[太陽]]的1540倍（{{solar radius|link=y}}），和亮度約為[[太陽亮度]]（{{solar luminosity|link=y}}）282,000倍。如果將它放置在[[太陽系]]的中心，該恆星的[[光球層]]將吞噬[[木星]]的軌道。

WOH G64被一個直徑約為一光年的光學厚塵埃包層包圍，其中包含由强恆星風產生，被驅逐物質的質量為3到9倍[[太陽質量]]<ref name=ohnaka>{{Cite journal | last1 = Ohnaka | first1 = K. | last2 = Driebe | first2 = T. | last3 = Hofmann | first3 = K. H. | last4 = Weigelt | first4 = G. | last5 = Wittkowski | first5 = M. | title = Resolving the dusty torus and the mystery surrounding LMC red supergiant WOH G64 | doi = 10.1017/S1743921308028858 | journal = Proceedings of the International Astronomical Union | volume = 4 | pages = 454–458 | year = 2009 | bibcode = 2009IAUS..256..454O | doi-access = free }}</ref>。

==發現史==
WOH G64是由[[本特·維斯特盧]]、奧蘭德（{{langx|en|Olander}}）和赫丁（{{langx|en|Hedin}}）在20世紀70年代發現的。與[[天鵝座NML]]一樣，這顆恆星名稱中的「WOH」來自其三位發現者的名字，但在這種情況下，它指的是LMC中的一系列巨星和超巨星<ref name="westerlund">{{Cite journal |last=Westerlund |first=B. E. |last2=Olander |first2=N. |last3=Hedin |first3=B. |year=1981 |title=Supergiant and giant M type stars in the Large Magellanic Cloud. |journal=[[Astronomy and Astrophysics Supplement Series]] |volume=43 |pages=267–295 |bibcode=1981A&AS...43..267W |issn=0365-0138}}</ref>。維斯特盧還發現了另一顆位於[[星座]][[天壇座]]的[[超星團]][[維斯特盧1]]中的著名大質量紅超巨星[[維斯特盧1-26]]<ref name=westerlund1987>{{Cite journal |last=Westerlund |first=B. E. |date=1987 |title=Photometry and spectroscopy of stars in the region of a highly reddened cluster in ARA |journal=[[Astronomy & Astrophysics]] |series=Supplement |issn=0365-0138 |volume=70 |issue=3 |pages=311–324 |bibcode=1987A&AS...70..311W}}</ref>。1986年，紅外觀測表明，它是一顆被氣體和塵埃包圍，被吸收了大約四分之三輻射的高亮度超巨星<ref name=elias/>。

2007年，使用[[甚大望遠鏡]]（VLT）的觀測者發現，WOH G64被一個環形雲包圍著<ref name=ohnaka/>。

== 距離 ==
因為它似乎在LMC中，因此假設WOH G64距離地球約{{convert|50,000|pc|ly|lk=on}}<ref name=levesque/>。WOH G64的[[蓋亞目錄#蓋亞DR2|蓋亞DR2]]發布的視差為{{val|-0.2280|0.0625|ul=mas}}，而此負視差不能提供可靠的距離<ref name=dr2/>。

== 變異性 ==
WOH G64在可見光的波長下，亮度有規律地變化超過一個數量級，主要週期約為800天<ref name=macho>{{cite journal|bibcode=2008AJ....136.1242F|arxiv=0808.1737|title=The Properties of Long-Period Variables in the Large Magellanic Cloud from MACHO|url=https://archive.org/details/sim_astronomical-journal_2008-09_136_3/page/1242|journal=The Astronomical Journal|volume=136|issue=3|pages=1242–1258|last1=Fraser|first1=Oliver J.|last2=Hawley|first2=Suzanne L.|last3=Cook|first3=Kem H.|year=2008|doi=10.1088/0004-6256/136/3/1242|s2cid=2754884}}</ref>。這顆恆星在可見波長下的消光幅度超過六星等，在紅外波長下的變化要小得多<ref name=levesque/>。它被描述為富含碳的[[米拉變星]]或[[長週期變星]]，必然是[[漸近巨星支|漸近巨星支星]]（AGB星），而不是超巨星<ref name=ogle>{{cite journal|bibcode=2009AcA....59..239S|title=The Optical Gravitational Lensing Experiment. The OGLE-III Catalog of Variable Stars. IV. Long-Period Variables in the Large Magellanic Cloud|journal=Acta Astronomica|volume=59|issue=3|pages=239|last1=Soszyñski|first1=I.|last2=Udalski|first2=A.|last3=Szymañski|first3=M. K.|last4=Kubiak|first4=M.|last5=Pietrzyñski|first5=G.|last6=Wyrzykowski|first6=Ł.|last7=Szewczyk|first7=O.|last8=Ulaczyk|first8=K.|last9=Poleski|first9=R.|year=2009|arxiv=0910.1354}}</ref>。其他研究人員已經證實了某些光譜帶的亮度變化，但尚不清楚實際的變化類型是什麼。光譜沒有發現明顯的變化<ref name=levesque/>。

== 物理性質 ==
[[File:WOH G64 Particular.jpg|thumb|left|upright=1.2|藝術家對WOH G64周圍塵土飛揚的圓環的印象（[[歐洲南方天文臺]]）]]

WOH G64的光譜類型為M5<ref name=levesque/>，但通常發現它具有更冷的光譜類型M7.5，這對於超巨星來說非常不尋常<ref name=vanloon/><ref name=elias/><ref name=davies2018/>。

WOH G64被歸類為極亮的M級超巨星，可能是LMC中最大的恆星，也是最亮和[[最冷恆星列表|最冷]]的紅超巨星<ref name=levesque/>。恆星的溫度和光度的組合使其位於[[赫羅圖]]的右上角。這顆恆星的演化狀態意味著，由於低密度、高輻射壓力和相對不透明的熱核聚變產物，它無法再保持大氣層{{citation needed|date=June 2020}}。它的平均質量損失率為每年3.1至{{val|5.8|e=-4|u={{solar mass}}}}，這是已知的最高值之一，甚至對於紅超巨星來說也是異常高的<ref name="steven">{{Cite journal |last=Goldman |first=Steven R. |last2=van Loon |first2=Jacco Th. |last3=Zijlstra |first3=Albert A. |last4=Green |first4=James A. |last5=Wood |first5=Peter R. |last6=Nanni |first6=Ambra |last7=Imai |first7=Hiroshi |last8=Whitelock |first8=Patricia A. |last9=Matsuura |first9=Mikako |last10=Groenewegen |first10=Martin A. T. |last11=Gómez |first11=José F. |display-authors=3 |date=February 2017 |title=The wind speeds, dust content, and mass-loss rates of evolved AGB and RSG stars at varying metallicity |journal=[[Monthly Notices of the Royal Astronomical Society]] |language=en |volume=465 |issue=1 |pages=403–433 |arxiv=1610.05761 |bibcode=2017MNRAS.465..403G |doi=10.1093/mnras/stw2708 |issn=0035-8711 |s2cid=11352637 |doi-access=free}}</ref><ref name="LMC-SMC">{{Cite journal|last1=de Wit|first1=S.|last2=Bonanos|first2=A.Z.|last3=Tramper|first3=F.|last4=Yang|first4=M.|last5=Maravelias|first5=G.|last6=Boutsia|first6=K.|last7=Britavskiy|first7=N.|last8=Zapartas|first8=E.|title=Properties of luminous red supergiant stars in the Magellanic Clouds|journal=[[Astronomy and Astrophysics]]|year=2023 |volume=669 |pages=17|doi=10.1051/0004-6361/202243394 |arxiv=2209.11239|bibcode=2023A&A...669A..86D |s2cid=252519285}}</ref>。

WOH G64 的參數不確定。根據假設球殼的光譜測量，這顆恆星最初被計算出的光度在{{solar luminosity|490,000 and 600,000}}之間，這表明初始質量至少為{{solar mass|40}}，因此半徑值在{{solar radius|2,575到3,000}}之間<ref name=vanloon/><ref name=elias/><ref name=monnier>{{cite journal|bibcode=2004ApJ...605..436M|arxiv=astro-ph/0401363|title=High-Resolution Imaging of Dust Shells by Using Keck Aperture Masking and the IOTA Interferometer|url=https://archive.org/details/sim_astrophysical-journal_2004-04-10_605_1/page/435|journal=The Astrophysical Journal|volume=605|issue=1|pages=436–461|last1=Monnier|first1=J. D|last2=Millan-Gabet|first2=R|last3=Tuthill|first3=P. G|last4=Traub|first4=W. A|last5=Carleton|first5=N. P|last6=Coudé Du Foresto|first6=V|last7=Danchi|first7=W. C|last8=Lacasse|first8=M. G|last9=Morel|first9=S|last10=Perrin|first10=G|last11=Porro|first11=I. L|last12=Schloerb|first12=F. P|last13=Townes|first13=C. H|year=2004|doi=10.1086/382218|s2cid=7851916}}</ref>。2018年的一次測量給出了{{Solar luminosity|432,000}}的光度和更高的有效溫度 {{val|3,500|ul=K|fmt=commas}}，這是基於光學和紅外[[光度測定 (天文學)|光度學]]，並假設來自周圍塵埃的球對稱輻射。這表明半徑為{{Solar radius|1,788}}<ref name="Groenewegen2018"/>{{efn|name=radius}}。

[[File:WOH G64 and The Sun.jpg|thumb|WOH G64與太陽的比較。|left]]

2007年使用[[甚大望遠鏡]]（VLT）進行的測量，基於周圍環面的輻射傳輸模型，得出這顆恆星的[[光度#測量|輻射熱光度]]為{{Solar luminosity|{{val|282,000|40,000|30,000|fmt=commas}}}}，根據[[有效溫度]]{{val|3,200|fmt=commas|ul=K}}的假設，初始質量為{{val|25|5|u={{solar mass|link=y}}}}，半徑約為{{Solar radius|1,730}}<ref name=ohnaka/>。2009年，[[艾米麗·萊維斯克|萊維斯克]]通過光學和近紫外[[光譜能量分佈]]的光譜擬合計算出3,400±25 K的有效溫度。採用 Ohnaka 光度和這個新溫度，給出的半徑為{{val|1,540|fmt=commas|u={{solar radius}}}}，但[[誤差範圍]]為5% 或 {{solar radius|77}}<ref name=levesque/>。這些物理參數與其它地方發現的最大的星系紅超巨星和超巨星一致，例如[[大犬座VY]]以及最冷、最亮和最大的冷超巨星的理論模型（例如 [[林極限]]或[[愛丁頓光度#漢弗萊斯-大衛森極限|漢弗萊斯-大衛森極限]]）<ref name=levesque/><ref name=vanloon/><ref name=ohnaka/>。忽略塵埃環面對重定向紅外輻射的影響，根據光度{{val|450,000|150,000|120,000|u={{solar luminosity}}|fmt=commas}}和有效溫度3,372 - {{val|3,400|fmt=commas|u=K}}，也得出了{{solar radius|1,990}}的估計值<ref name=levesque/>。

=== 光譜特徵 ===
WOH G64被發現是[[羥自由基|OH]]、[[水]]和{{chem|link=一氧化矽|SiO}} [[天文物理邁射]]發射源，這是 [[OH/IR星|OH/IR超巨星]]的典型特徵<ref name=levesque/>。它顯示了不尋常的星雲發射[[光譜]]；熱氣體富含氮，其[[徑向速度]]比恆星的正值大得多<ref name=levesque/>。恆星大氣在中紅外波長中產生強矽酸鹽[[吸收帶]]，並伴有由於高激發的[[一氧化碳]]而產生的線發射<ref>{{Cite journal |last1=Matsuura |first1=Mikako |last2=Sargent |first2=B. |last3=Swinyard |first3=Bruce |last4=Yates |first4=Jeremy |last5=Royer |first5=P. |last6=Barlow |first6=M. J. |last7=Boyer |first7=Martha |last8=Decin |first8=L. |last9=Khouri |first9=Theo |last10=Meixner |first10=Margaret |last11=van Loon |first11=Jacco Th. |last12=Woods |first12=Paul M. |date=1 November 2016 |title=The mass-loss rates of red supergiants at low metallicity: detection of rotational CO emission from two red supergiants in the Large Magellanic Cloud |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=462 |issue=3 |pages=2995–3005 |doi=10.1093/mnras/stw1853 |doi-access=free |issn=0035-8711|arxiv=1608.01729 }}</ref>。

== 可能的伴侶 ==
WOH G64可能有一個晚期的[[O型主序星]]伴星，其[[光度#測量|輻射熱星等]]為 -7.5 或光度為{{solar luminosity|100,000}}，這將使 WOH G64成為[[聯星]]。儘管這一觀察結果尚未得到證實，而且其間的塵埃雲使對這顆恆星的研究變得非常困難<ref name=levesque/>。

== 相關條目 ==
*{{link-en|B90 (恆星)|B90 (star)}}：大麥哲倫星系中的另一顆紅超巨星。
*[[大犬座VY]]：被認為是銀河系中最大的恆星，1420倍太陽半徑。
*[[R136a1]]：已知質量最大、亮度最高的恆星之一。
*[[天鹅座NML]]：1650倍太陽半徑
*[[麒麟座V838]]：1570倍太陽半徑(帕羅馬測試干涉儀的觀測)
*[[人马座VX]]：1520倍太陽半徑
*[[人马座KW]]：1460倍太陽半徑
*[[天鹅座KY]]：1420～2850倍太陽半徑
*[[维斯特卢1-26]]：1520～1580倍太陽半徑
*[[盾牌座UY]]：1708倍太阳半径，已知最大恒星。
{| border= "1"
|-
| < 2. [[天鹅座NML]] 
| 4. [[维斯特卢1-26]]>
|}

== 註解 ==
{{notelist|refs=

{{efn | name=radius |應用[[斯特凡-波茲曼定律]]，並依據[[太陽]]的[[有效溫度]]為5,772&nbsp;[[開爾文|K]]：
:<math>\sqrt{(5772/3500)^4 * 432,190} = 1787.94\ R\odot</math>}}

}}

== 參考資料 ==
{{reflist|refs=

<ref name=2mass>{{cite journal |bibcode=2003yCat.2246....0C |title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) |journal=CDS/ADC Collection of Electronic Catalogues |pages=II/246 |volume=2246 |last1=Cutri |first1=Roc M. |last2=Skrutskie |first2=Michael F. |last3=Van Dyk |first3=Schuyler D. |last4=Beichman |first4=Charles A. |last5=Carpenter |first5=John M. |last6=Chester |first6=Thomas |last7=Cambresy |first7=Laurent |last8=Evans |first8=Tracey E. |last9=Fowler |first9=John W. |last10=Gizis |first10=John E. |last11=Howard |first11=Elizabeth V. |last12=Huchra |first12=John P. |last13=Jarrett |first13=Thomas H. |last14=Kopan |first14=Eugene L. |last15=Kirkpatrick |first15=J. Davy |last16=Light |first16=Robert M. |last17=Marsh |first17=Kenneth A. |last18=McCallon |first18=Howard L. |last19=Schneider |first19=Stephen E. |last20=Stiening |first20=Rae |last21=Sykes |first21=Matthew J. |last22=Weinberg |first22=Martin D. |last23=Wheaton |first23=William A. |last24=Wheelock |first24=Sherry L. |last25=Zacarias |first25=N. |year=2003 |url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246 |access-date=2024-11-29 |archive-date=2021-04-21 |archive-url=https://web.archive.org/web/20210421020651/https://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II%2F246 |dead-url=no }}</ref>

<ref name="elias">{{Cite journal |last=Elias |first=J. H. |last2=Frogel |first2=J. A. |last3=Schwering |first3=P. B. W. |date=March 1986 |title=Two supergiants in the Large Magellanic Cloud with thick dust shells |url=https://archive.org/details/sim_astrophysical-journal_1986-03-15_302_2/page/n181 |journal=[[The Astrophysical Journal]] |language=en |volume=302 |pages=675 |bibcode=1986ApJ...302..675E |doi=10.1086/164028 |issn=0004-637X |hdl-access=free |hdl=1887/6514}}</ref>

<ref name=dr2>{{cite Gaia DR2|4661527262798576768}}</ref>

<ref name=vanloon>{{cite journal|bibcode=2005A&A...438..273V|arxiv=astro-ph/0504379|title=An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars|journal=[[Astronomy and Astrophysics]]|volume=438|pages=273–289|last1=Van Loon|first1=J. Th.|last2=Cioni|first2=M.-R. L.|last3=Zijlstra|first3=A. A.|last4=Loup|first4=C.|year=2005|issue=1|doi=10.1051/0004-6361:20042555|s2cid=16724272}}</ref>

}}

== 外部連結 ==
{{Commons category}}

{{Stars of Dorado}}

{{DEFAULTSORT:WOH G64}}
[[Category:大麥哲倫星系中的恆星]]
[[Category:M型超巨星]]
[[Category:大麥哲倫星系]]
[[Category:銀河系外恆星]]
[[Category:2MASS天體|J04551048-6820298]]
[[Category:劍魚座]]
[[Category:IRAS星表天體]]
[[Category:發射線星]]
[[Category:TIC天體]]