{{위키데이터 속성 추적}}
아래 표는 지금까지 '''관측된 별들 중 [[질량]]이 큰 것들'''을 순서대로 정렬한 것이다. 단위는 [[태양질량]]({{태양질량|link=y}})이다.

==불확실성과 주의사항==
아래에 나열된 대부분의 질량은 논쟁의 여지가 있으며 현재 연구 주제이므로 계속 검토되고 질량 및 기타 특성이 지속적으로 수정된다. 실제로 아래 표에 나열된 질량 중 상당수는 [[별]]의 [[유효온도|온도]]와 절대 밝기에 대한 어려운 측정을 사용하는 이론을 통해 추론되었다. 아래 나열된 질량은 모두 불확실하다. 이론과 측정 모두 현재 지식과 기술의 한계를 밀어붙이고 있으며 이론과 측정 모두 부정확할 수 있다. 예를 들어 [[세페우스자리 VV]]는 사용된 별의 특성에 따라 {{태양질량|25–40|link=y}} 또는 {{태양질량|100}} 사이일 수 있다.

[[파일:Dust disk around massive star.jpg|thumb|무거운 별을 가리는 주의의 원반의 작가의 표현.]]

===거리와 먼지로 인한 가려짐의 문제===
거대한 별은 드물기 때문에 [[천문학자]]들은 이를 찾으려면 [[지구]]에서 아주 멀리 떨어진 곳을 관찰해야 하며 나열된 모든 별은 수천 광년 떨어져 있으므로 측정이 어렵다. 멀리 떨어져 있는 것 외에도 엄청난 질량을 가진 많은 별들은 극도로 강력한 [[항성풍]]에 의해 생성된 가스 구름으로 둘러싸여 있으며 주변 가스는 이미 얻기 어려운 항성의 온도와 밝기 측정을 방해하여 내부 화학 조성과 구조를 추정하는 문제를 크게 복잡하게 만든다.{{efn|일부 방법의 경우 화학 조성을 다르게 결정하면 질량 추정치가 달라진다.}} 이러한 방해로 인해 매개변수 계산이 어려워진다.

[[파일:EtaCarinae.jpg|thumb|right|[[용골자리 에타]]는 [[호문쿨루스 성운|이중의 둥근 돌출부 모양 먼지 구름]] 속에 숨겨진 밝은 점으로 [[바이어 명명법|바이어 부호]]를 받은 가장 무거운 별이다. 적어도 지난 수십 년 동안 두 개의 별인 것이 발견되었다.]]
먼지의 가림과 먼 거리로 인해 별이 단일 초중량 별인지 아니면 [[다중성계]]인지 판단하기가 어렵다. 아래에 나열된 많은 "별"들은 실제로 망원경으로 구별하기에는 너무 가깝게 공전하는 두 개 이상의 별이라 각 별도 그 자체로 무겁지만 이 목록에 있거나 맨 위에 있을 정도로 "초중량"은 아닐 수 있다. 다른 조합도 가능한데 예를 들어 하나 이상의 작은 동반성이 있는 초중량 별이거나 하나 이상의 거대한 별이 있을 수 있지만 주변 먼지 내부를 볼 수 없으면 진실을 알기가 어렵다.

보다 전체적으로 항성에 대한 통계에 따르면 질량 상한은 100-200&nbsp;태양질량 범위에 있는 것으로 나타나므로<ref>{{컨퍼런스 인용|last1=van Marle |first1=A.J. |last2=Owocki |first2=S.P. |last3=Shaviv |first3=N.J. |date=March 2008 |title=Continuum-driven winds from super-Eddington stars: A tale of two limits |conference=First Stars&nbsp;III: First Stars&nbsp;III Conference. AIP Conference Proceedings |series=AIP Conference Proceedings |location=Santa Fe, NM |volume=990 |pages=250–253 |arxiv=0708.4207 |bibcode=2008AIPC..990..250V |doi=10.1063/1.2905555 |issn=0094-243X |s2cid=118364586}}</ref> 이 범위를 초과하는 모든 질량 추정치는 의심스럽다.

===드문 신뢰 가능한 추정치===
식쌍성은 질량이 어느 정도 확실하게 추정되는 유일한 별이지만 아래 표에 나열된 거의 모든 질량은 간접적인 방법으로 추론되었다. 표에 있는 천체의 질량 중 소수만이 식쌍성계를 이용하여 결정되었다.

수록된 질량 중 신뢰도가 가장 높은 것은 식쌍성 [[NGC 3603-A1]], [[WR 21a]] 및 [[WR 20a]]의 질량이다. 세 천체 모두 궤도 측정을 통해 질량을 얻었는데{{efn|쌍성의 경우 [[케플러의 행성운동법칙]]을 사용하여 궤도 운동을 조사함으로써 두 별의 개별 질량을 측정하는 것이 가능하다.}} 여기에는 [[시선속도]]와 광도곡선을 측정하는 작업이 포함된다. 시선속도는 기울기에 따라 질량의 최소값만을 산출하지만 식쌍성의 광도곡선은 누락된 정보, 즉 우리 시선에 대한 궤도 경사각을 제공한다.

===항성진화의 관련성===
일부 별은 한때 오늘날보다 더 무거웠을 수도 있고 많은 큰 별들이 상당한 질량 손실(어쩌면 태양 질량의 수십 배 까지도)을 겪었을 가능성이 높다. 이 질량은 뜨거운 [[광구]]에 의해 성간 공간으로 이동하는 고속 항성풍인 [[슈퍼윈드]]에 의해 방출되었을 수 있다. 이 과정은 근처의 성간 물질과 상호 작용하고 수소나 헬륨보다 무거운 원소를 해당 지역에 주입하는 별 주위에 확대된 확장된 외피를 형성한다.{{efn|무거운 별에서 발생하는 [[슈퍼윈드]]는 [[행성상성운]]을 형성하는 [[점근거성열|점근거성가지성]]에서 발생하는 [[슈퍼윈드]]와 유사하다. 이 별들의 잔해는 행성상 성운의 (엄밀하게는 별이 아닌) [[백색왜성]] 핵이 된다.}}

목록에 존재했지만 더 이상 별로 존재하지 않거나 [[의사 초신성]]인 별도 있으며 오늘날 우리는 그 잔해만을 볼 수 있다.{{efn|잔해의 예시에 대해서는 [[극초신성]]과 [[초신성 잔해]] 참조}} 이러한 파괴적인 사건의 원인이 된 전구별의 질량은 초신성 유형과 방출된 에너지를 통해 추정할 수 있지만 해당 질량은 여기에 나열되어 있지 않다(아래 [[#블랙홀|§ 블랙홀]] 참조).

===질량 한계===
별의 질량이 얼마나 클 수 있는지에 대한 두 가지 관련 이론적 한계가 있는데 바로 강착 한계와 에딩턴 질량 한계다. 강착 한계는 별 형성과 관련이 있는데 [[원시별]]에 약 120 {{태양질량|link=y}}이 강착된 후에는 발생하는 열이 더 이상 들어오는 물질을 밀어낼 만큼 충분히 뜨거워져야 하고 실제로 원시별은 새로운 물질을 얻는만큼 빠르게 물질을 잃는 지점에 도달한다. [[에딩턴 한계]]는 이미 형성된 별의 중심에서 나오는 광압에 기초하는데 질량이 ~150 {{태양질량}}을 넘어 증가하면 [[항성의 종족|종족I]] 별의 중심에서 방출되는 빛의 강도는 바깥쪽으로 밀어내는 광압이 안으로 끌어당기는 중력을 이겨내기에 충분해지고 이에 따라 중력이 안쪽으로 당기고 이에 따라 별 표면의 물질은 자유롭게 우주로 떠내려갈 수 있게 된다.

====강착 한계====
천문학자들은 [[원시별]]이 120 {{태양질량|link=y}} 이상의 크기로 성장하면 급격한 일이 일어나야 한다는 가설을 오랫동안 생각해 왔다.<ref name="Maeder">{{저널 인용 |last1=Maeder |first1=A. |last2=Georgy |first2=C. |last3=Meynet |first3=G. |last4=Ekström |first4=S. |date=March 2012 |title=On the Eddington limit and Wolf-Rayet stars |url=http://www.aanda.org/10.1051/0004-6361/201118328 |journal=Astronomy & Astrophysics |volume=539 |pages=A110 |arxiv=1201.5013 |bibcode=2012A&A...539A.110M |doi=10.1051/0004-6361/201118328 |issn=0004-6361 |s2cid=119230088}}</ref> 매우 초기의 [[항성종족|종족III]] 별에 대해서는 한계가 확장될 수 있고 정확한 값은 불확실하지만 150-200{{태양질량}} 이상의 별이 여전히 존재한다면 [[항성진화]]에 대한 현재 이론에 도전하게 될 것이다.

천문학자들은 현재 [[우리은하]]에서 가장 밀도가 높은 것으로 알려진 성단인 [[아치스 성단]]을 연구하면서 해당 성단에 약 150 {{태양질량}}을 초과하는 별이 없음을 확인했다.

[[파일:Grand star-forming region R136 in NGC 2070 (captured by the Hubble Space Telescope).jpg|thumb|right|[[R136]] 성단은 젊고 뜨겁고 푸른 별들로 이루어진 비정상적으로 밀집된 성단이다.]]
이 한계를 초과하는 희귀 초중량별(예: [[R136]] 성단의 별)은 다음 안으로 설명될 수 있다: 젊고 불안정한 [[항성계#트라페지아|다중성계]]에서 [[쌍성계|가까운 궤도]]에 있는 무거운 별 쌍 중 일부는 충돌을 일으킬 수 있는 비정상적인 상황이 발생하면 특정 경우 때때로 충돌하고 합쳐져야 한다.<ref name=bannerjee>{{저널 인용 |last1=Banerjee |first1=Sambaran |last2=Kroupa |first2=Pavel |last3=Oh |first3=Seungkyung |date=21 October 2012 |title=The emergence of super-canonical stars in R136-type starburst clusters: Super-canonical stars in R136 |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=426 |issue=2 |pages=1416–1426 |arxiv=1208.0826 |bibcode=2012MNRAS.426.1416B |doi=10.1111/j.1365-2966.2012.21672.x |issn=0035-8711 |s2cid=119202197 |lang=en}}</ref>

====에딩턴 질량 한계====
{{본문|에딩턴 한계}}
항성 질량에 대한 [[아서 스탠리 에딩턴|에딩턴]]의 한계는 광압 때문에 발생하는데 충분히 질량이 큰 별의 경우 별 중심핵의 [[핵융합]]에 의해 생성된 [[복사 에너지]]의 바깥으로 밀어내는 힘은 자체 중력이 안으로 끌어당기는 힘을 초과하게 된다. 이 효과가 시작되는 가장 낮은 질량이 ''[[에딩턴 한계]]''다.

질량이 더 큰 별은 중심핵의 에너지 생성률이 더 높으며 무거운 별의 광도는 질량 증가보다 훨씬 더 증가한다. [[에딩턴 한계]]는 별이 스스로 해체되거나 적어도 내부 에너지 생성을 더 낮고 유지 가능한 속도로 줄일 수 있을 만큼 충분한 질량을 버려야 하는 지점이다. 실제 한계점은 별의 가스가 얼마나 불투명한지에 따라 달라지며 금속이 풍부한 [[항성의 종족|종족I]] 별은 금속이 부족한 [[항성의 종족|종족II]] 별보다 질량 한계가 더 낮다. 소멸되기 전에는 금속이 없는 가상의 [[항성의 종족|종족III]] 별은 약 300 {{태양질량}} 정도의 가장 높은 허용 질량을 가졌을 것이다.

이론적으로 더 무거운 별은 항성 물질의 유출로 인한 질량 손실로 인해 스스로를 지탱할 수 없다. 실제로 이론적인 [[에딩턴 한계]]는 광도가 높은 별에 대해 수정되어야 하며 경험적인 [[험프리스-데이비슨 한계]]가 대신 사용된다.<ref name=HD>{{저널 인용 |last1=Ulmer |first1=Andrew |last2=Fitzpatrick |first2=Edward L. |date=September 1998 |title=Revisiting the modified Eddington limit for massive stars |journal=The Astrophysical Journal |language=en |volume=504 |issue=1 |pages=200–206 |arxiv=astro-ph/9708264 |bibcode=1998ApJ...504..200U |doi=10.1086/306048 |issn=0004-637X |s2cid=14916494}}</ref>

== 목록 ==

{| class="wikitable floatright" style="width: 170px;"
|+'''범례'''
|-
| style="background: {{항성-색깔|WC}};" align="center" | [[볼프-레이에별]]
|-
| style="background: {{항성-색깔|WN}};" align="center" | [[밝은 청색변광성]]
|-
| style="background: {{항성-색깔|O}};"  align="center" | [[O형 항성]]
|-
| style="background: {{항성-색깔|B}};"  align="center" | [[B형 주계열성|B형 항성]]
|-
|}
다음 두 목록은 [[산개성단]], [[항성운동학|OB 성협]], [[전리수소영역|H II 영역]]의 별을 포함하여 알려진 별 중 몇 가지를 수록한다. 목록의 상당수의 별들은 높은 광도에도 불구하고 맨눈으로 관찰하기에는 너무 멀리 떨어져 있으며 적어도 맨눈으로 가끔 볼 수 있는 별은 겉보기 등급(6.5 이상)이 파란색으로 강조되어 있다.

첫 번째 목록은 60&nbsp;{{태양질량}} 이상으로 추정되는 별으로 그 중 대부분이 수록되며 두 번째 목록에는 비교를 위해 60&nbsp;{{태양질량}} 미만의 주목할만한 별이 수록되어 있다. 데이터의 불확실성에 대한 정보를 제공하기 위해 각 별의 질량을 결정하는 데 사용되는 방법이 포함되어있으며 쌍성의 질량은 훨씬 더 정확하게 결정될 수 있다. 아래 나열된 질량은 별의 초기 질량이 아닌 현재 질량이다.{{미완성 목록|date=January 2016}}<!-- 삭제하지 마세요, 이 목록은 인류가 알려진 우주 전체를 관측하기 전에는 완성될 수 없습니다. -->

{| class="wikitable sortable"
|+<big>'''60 {{태양질량|link=y}} 이상의 항성들'''<big>
|-
! 항성 이름
! [[질량]]
({{태양질량|link=y}}, [[태양]] = 1)
! 대략 태양계로부터의 거리([[광년]])
! [[겉보기등급]]
! [[표면온도|유효온도]] ([[켈빈|K]])
! 분석 방식
! 링크
! 참고문헌
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[BAT99-98]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|226
|165,000
|13.37
|45,000
|분광법
|{{SIMBAD link|BAT99+98|SIMBAD}}
|<ref name="hainich">{{저널 인용|last1=Hainich |first1=R. |last2=Rühling |first2=U. |last3=Todt |first3=H.|last4=Oskinova|first4=L. M.|last5=Liermann|first5=A.|last6=Gräfener|first6=G.|last7=Foellmi|first7=C.|last8=Schnurr|first8=O.|last9=Hamann|first9=W.-R. |display-authors=6 |date=May 2014|title=The Wolf-Rayet stars in the Large Magellanic Cloud. A comprehensive analysis of the WN class |journal=Astronomy & Astrophysics |volume=565 |page=A27 |arxiv=1401.5474 |bibcode=2014A&A...565A..27H|doi=10.1051/0004-6361/201322696|issn=0004-6361|s2cid=55123954}}</ref><ref name="Doran2013">{{저널 인용|last1=Doran |first1=E.I. |last2=Crowther |first2=P.A.|last3=de Koter |first3=A. |last4=Evans |first4=C.J. |last5=McEvoy |first5=C. |last6=Walborn |first6=N.R. |last7=Bastian |first7=N. |last8=Bestenlehner |first8=J.M. |last9=Gräfener |first9=G. |last10=Herrero |first10=A. |last11=Köhler |first11=K. |first15=H. |first18=J.Th. |last19=Vink|last18=van Loon |first17=W.D. |last17=Taylor |first16=F.R.N. |last14=Puls |last16=Schneider |last15=Sana |first14=J. |first13=F. |last13=Najarro|first12=J. |last12=Maíz Apellániz |first19=J.S. |display-authors=6 |date=October 2013 |title=The VLT-FLAMES Tarantula Survey: XI. A census of the hot luminous stars and their feedback in 30 Doradus|journal=Astronomy & Astrophysics |volume=558 |page=A134 |arxiv=1308.3412 |bibcode=2013A&A...558A.134D|doi=10.1051/0004-6361/201321824 |issn=0004-6361 |s2cid=118510909}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[R136a1]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|196
|163,000
|12.23
|46,000
|항성진화 모델
|{{SIMBAD link|RMC136a1|SIMBAD}}
|<ref name=":0">{{저널 인용|last1=Bestenlehner |first1=Joachim M. |last2=Crowther |first2=Paul A. |last3=Caballero-Nieves |first3=Saida M. |last4=Schneider |first4=Fabian R. N. |last5=Simón-Díaz |first5=Sergio |last6=Brands |first6=Sarah A. |last7=de Koter |first7=Alex |last8=Gräfener |first8=Götz |last9=Herrero |first9=Artemio |last10=Langer |first10=Norbert |last11=Lennon |first11=Daniel J. |date=2020-12-01 |title=The R136 star cluster dissected with Hubble Space Telescope/STIS - II. Physical properties of the most massive stars in R136 |url=https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.1918B |journal=Monthly Notices of the Royal Astronomical Society |volume=499 |issue=2 |pages=1918–1936 |doi=10.1093/mnras/staa2801 |arxiv=2009.05136 |bibcode=2020MNRAS.499.1918B |issn=0035-8711}}</ref><ref name=":1">{{저널 인용|last1=Kalari |first1=Venu M. |last2=Horch |first2=Elliott P. |last3=Salinas |first3=Ricardo |last4=Vink |first4=Jorick S. |last5=Andersen |first5=Morten |last6=Bestenlehner |first6=Joachim M. |last7=Rubio |first7=Monica |date=2022-07-26 |title=Resolving the Core of R136 in the Optical |journal=The Astrophysical Journal |volume=935 |issue=2 |page=162 |doi=10.3847/1538-4357/ac8424 |arxiv=2207.13078 |bibcode=2022ApJ...935..162K |s2cid=251067072 |doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[멜닉 42]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|189
|163,000
|12.78
|47,300
|분광법
|{{SIMBAD link|Cl*+NGC+2070+MEL+42|SIMBAD}}
|<ref name="best">{{저널 인용|last1=Bestenlehner |first1=J.M. |last2=Gräfener |first2=G. |last3=Vink |first3=J.S. |last4=Najarro |first4=F. |last5=de Koter |first5=A. |last6=Sana |first6=H. |last7=Evans |first7=C.J. |last8=Crowther |first8=P.A. |last9=Hénault-Brunet |first9=V. |last10=Herrero |first10=A. |last11=Langer |first11=N. |last12=Schneider |first12=F.R.N. |last13=Simón-Díaz |first13=S. |first14=W.D. |last14=Taylor |first15=N.R. |last15=Walborn |display-authors=6 |date=October 2014 |title=The VLT-FLAMES Tarantula Survey: XVII. Physical and wind properties of massive stars at the top of the main sequence |journal=Astronomy & Astrophysics |volume=570 |page=A38 |arxiv=1407.1837 |bibcode=2014A&A...570A..38B |doi=10.1051/0004-6361/201423643 |issn=0004-6361 |s2cid=118606369}}</ref><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[VFTS 1022]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|178
|164,000
|13.47
|42,200
|분광법
|{{SIMBAD link|VFTS+1022|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[웨스터하우트 51]]-57 ([[웨스터하우트 51]]에 존재)
|160
|20,000
|16.66<br/>{{small|(J&nbsp;대역)}}
|42,700
|항성진화 모델
|
|<ref name=Bik>{{저널 인용|last1=Bik |first1=A. |last2=Henning |first2=Th. |last3=Wu |first3=S.-W. |last4=Zhang |first4=M. |last5=Brandner |first5=W. |last6=Pasquali |first6=A. |last7=Stolte |first7=A. |date=April 2019 |title=Near-infrared spectroscopy of the massive stellar population of W51: evidence for multi-seeded star formation |journal=Astronomy & Astrophysics |volume=624 |page=A63 |arxiv=1902.05460 |bibcode=2019A&A...624A..63B |doi=10.1051/0004-6361/201935061 |issn=0004-6361 |s2cid=118711844 }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[R136a3]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|155
|163,000
|12.97
|50,000
|항성진화 모델
|{{SIMBAD link|RMC136a3|SIMBAD}}
|<ref name=":0" /><ref name=":1"/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[VFTS 682]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|153
|164,000
|16.08
|52,200
|분광법
|{{SIMBAD link|VFTS+682|SIMBAD}}
|<ref name="bagnulo2020">{{저널 인용|last1=Bagnulo |first1=S. |last2=Wade |first2=G.A. |last3=Nazé |first3=Y. |last4=Grunhut |first4=J.H. |last5=Shultz |first5=M.E. |last6=Asher |first6=D.J. |last7=Crowther |first7=P.A. |last8=Evans |first8=C.J. |last9=David-Uraz |first9=A. |last10=Howarth |first10=I.D. |last11=Morrell |first11=N. |last12=Munoz |first12=M.S. |last13=Neiner |first13=C. |last14=Puls |first14=J. |last15=Szymański |first15=M.K. |last16=Vink |first16=J.S. |display-authors=6  |date=March 2020|title=A search for strong magnetic fields in massive and very massive stars in the Magellanic Clouds|journal=Astronomy & Astrophysics |volume=635 |page=A163 |arxiv=2002.12061 |bibcode=2020A&A...635A.163B |doi=10.1051/0004-6361/201937098 |issn=0004-6361|s2cid=211532767}}</ref><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[HD 15558]] A ([[하트 성운]]의 [[IC 1805]]에 존재)
|152
|24,400
|7.87<br/>{{small|(연성계 전체)}}
|39,500
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|HD+15558|SIMBAD}}
|<ref name="debecker">{{저널 인용|last1=De Becker |first1=M. |last2=Rauw |first2=G. |last3=Manfroid |first3=J. |last4=Eenens |first4=P. |date=September 2006 |title=Early-type stars in the young open cluster IC&nbsp;1805: II. The probably single stars HD&nbsp;15570 and HD&nbsp;15629, and the massive binary/triple system HD&nbsp;15558 |journal=Astronomy & Astrophysics |volume=456 |issue=3 |pages=1121–1130 |arxiv=astro-ph/0606379 |bibcode=2006A&A...456.1121D |doi=10.1051/0004-6361:20065300|issn=0004-6361|s2cid=16519684}}</ref><ref name=ducati>{{보고서 인용|last1=Ducati |first1=J.R. |year=2002 |title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system |publisher=CDS/ADC |series=Collection of Electronic Catalogues |volume=2237 |bibcode=2002yCat.2237....0D |s2cid=118191108}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[R136a2]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|151
|163,000
|12.34
|50,000
|항성진화 모델
|{{SIMBAD link|RMC136a2|SIMBAD}}
|<ref name=":0"/><ref name=":1"/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[웨스터하우트 51]]-3 ([[웨스터하우트 51]]에 존재)
|148
|20,000
|17.79<br/>{{small|(J&nbsp;대역)}}
|39,800
|항성진화 모델
|{{SIMBAD link|2MASS+J19234283%2B1430277|SIMBAD}}
|<ref name=Bik/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[멜닉 34]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|147
|163,000
|13.09<br/>{{small|(연성계 전체)}}
|53,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|Cl*+NGC+2070+MEL+34|SIMBAD}}
|<ref name="tehrani">{{저널 인용|last1=Tehrani |first1=Katie A. |last2=Crowther |first2=Paul A. |last3=Bestenlehner |first3=Joachim M. |last4=Littlefair|first4=Stuart P. |last5=Pollock |first5=A.M.T. |last6=Parker |first6=Richard J. |last7=Schnurr |first7=Olivier |date=1 April 2019 |title=Weighing Melnick&nbsp;34: the most massive binary system known |journal=Monthly Notices of the Royal Astronomical Society |lang=en |volume=484 |issue=2 |pages=2692–2710 |arxiv=1901.04769 |bibcode=2019MNRAS.484.2692T|doi=10.1093/mnras/stz147|issn=0035-8711|s2cid=119069481}}</ref><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[VFTS 482]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|145
|164,000
|12.95
|42,200
|분광법
|{{SIMBAD link|VFTS+482|SIMBAD}}
|<ref name="best"/><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[R136c]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|142
|163,000
|13.43
|51,000
|항성진화 모델
|{{SIMBAD link|RMC136c|SIMBAD}}
|<ref name="schneider2018">{{저널 인용|last1=Schneider |first1=F.R.N. |last2=Sana |first2=H. |last3=Evans |first3=C.J. |last4=Bestenlehner |first4=J.M. |last5=Castro |first5=N. |last6=Fossati |first6=L. |last7=Gräfener |first7=G. |last8=Langer |first8=N. |last9=Ramírez-Agudelo |first9=O.H. |last10=Sabín-Sanjulián |first10=C. |last11=Simón-Díaz |first11=S. |last12=Tramper |first12=F. |last13=Crowther |first13=P.A. |last14=de Koter |first14=A. |last15=de Mink |first15=S.E. |last16=Dufton |first16=P.L. |last17=Garcia |first17=M. |last18=Gieles |first18=M. |last19=Hénault-Brunet |first19=V. |last20=Herrero |first20=A. |last21=Izzard |first21=R.G. |last22=Kalari |first22= V. |last23=Lennon |first23= D.J. |last24=Maíz Apellániz |first24=J. |last25=Markova |first25=N. |last26=Najarro |first26=F. |last27=Podsiadlowski |first27=Ph. |last28=Puls |first28=J. |last29=Taylor |first29= W.D. |last30=van Loon |first30= J.Th. |last31=Vink |first31=J.S. |last32=Norman |first32=C.  |display-authors=6 |date=5 January 2018 |title=An excess of massive stars in the local 30 Doradus starburst |journal=Science |language=en |volume=359 |issue=6371 |pages=69–71 |arxiv=1801.03107|bibcode=2018Sci...359...69S |doi=10.1126/science.aan0106 |pmid=29302009 |issn=0036-8075 |s2cid=206658504}}</ref><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[VFTS 1021]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|141
|164,000
|13.35
|39,800
|분광법
|{{SIMBAD link|VFTS+1021|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[LH 10]]-3209 A ([[대마젤란 은하]]의 [[NGC 1763]]에 존재)
|140
|160,000
|11.859<br/>{{small|(연성계 전체)}}
|42,500
|분광법
|{{SIMBAD link|PGMW+3209|SIMBAD}}
|<ref name="fulltext">{{저널 인용|last1=Walborn|first1=Nolan R.|last2=Howarth|first2=Ian D.|last3=Lennon|first3=Daniel J.|last4=Massey|first4=Philip|last5=Oey|first5=M. S.|last6=Moffat|first6=Anthony F. J.|last7=Skalkowski|first7=Gwen|last8=Morrell|first8=Nidia I.|last9=Drissen|first9=Laurent|last10=Parker|first10=Joel Wm. |display-authors=6 |date=May 2002|title=A New Spectral Classification System for the Earliest O Stars: Definition of Type O2|journal=The Astronomical Journal|volume=123|issue=5|pages=2754–2771|bibcode=2002AJ....123.2754W|doi=10.1086/339831|issn=0004-6256|s2cid=122127697|url=http://sedici.unlp.edu.ar/handle/10915/84631 |doi-access=free}}</ref><ref name=Bonanos>{{저널 인용|last1=Bonanos |first1=A.Z. |last2=Massa |first2=D.L. |last3=Sewilo |first3=M. |last4=Lennon |first4=D.J. |last5=Panagia |first5=N. |last6=Smith |first6=L.J.|last7=Meixner |first7=M. |last8=Babler |first8=B.L. |last9=Bracker |first9=S. |last10=Meade |first10=M.R. |last11=Gordon |first11=K.D. |display-authors=6  |date=1 October 2009 |title=Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud|journal=The Astronomical Journal|volume=138|issue=4|pages=1003–1021|arxiv=0905.1328|bibcode=2009AJ....138.1003B|doi=10.1088/0004-6256/138/4/1003|issn=0004-6256|s2cid=14056495|last12=Hora|last13=Indebetouw|last14=Whitney|first12=J. L.|first13=R.|first14=B. A.}}</ref><ref group=lower-alpha name=Binary/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[VFTS 506]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|138
|164,000
|13.31
|47,300
|분광법
|{{SIMBAD link|VFTS+506|SIMBAD}}
|<ref name="bagnulo2020"/><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[멜닉 34]] B ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|136
|163,000
|13.09<br/>{{small|(연성계 전체)}}
|53,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|Cl*+NGC+2070+MEL+34|SIMBAD}}
|<ref name="tehrani" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[웨스터하우트 51]]<nowiki/>d ([[웨스터하우트 51]]에 존재)
|135
|20,000
|15.11<br/>{{small|(J&nbsp;대역)}}
|42,700
|항성진화 모델
|
|<ref name=Bik/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[VFTS 545]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|133
|164,000
|13.32
|47,300
|분광법
|{{SIMBAD link|VFTS+545|SIMBAD}}
|<ref name="best" /><ref name="Doran2013"/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[NGC 3603-B|HD 97950 B]] ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43b)
|132
|24,800
|11.33
|42,000
|분광법
|{{SIMBAD link|HD+97950B|SIMBAD}}
|<ref name="crowther">{{저널 인용|last1=Crowther |first1=Paul A. |last2=Schnurr |first2=Olivier |last3=Hirschi|first3=Raphael |last4=Yusof |first4=Norhasliza|last5=Parker |first5=Richard J. |last6=Goodwin |first6=Simon P. |last7=Kassim |first7=Hasan Abu |date=21 October 2010|title=The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M⊙ stellar mass limit|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=408|issue=2|pages=731–751|arxiv=1007.3284|bibcode=2010MNRAS.408..731C|doi=10.1111/j.1365-2966.2010.17167.x|issn=0035-8711|s2cid=53001712}}</ref><ref name="melena2008">{{저널 인용|last1=Melena |first1=Nicholas W. |last2=Massey|first2=Philip|last3=Morrell|first3=Nidia I. |last4=Zangari |first4=Amanda M. |date=1 March 2008 |title=The massive star content of NGC 3603 |journal=[[The Astronomical Journal]] |volume=135 |issue=3 |pages=878–891 |arxiv=0712.2621 |bibcode=2008AJ....135..878M |doi=10.1088/0004-6256/135/3/878 |issn=0004-6256|s2cid=16765414}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[HD 269810]] ([[대마젤란 은하]]의 [[NGC 2029]]에 존재)
|130
| 163,000
|12.22
|52,500
|분광법
|{{SIMBAD link|HD+269810|SIMBAD}}
|<ref name="evans">{{저널 인용|last1=Evans|first1=C.J. |last2=Walborn |first2=N.R. |last3=Crowther |first3=P.A. |last4=Hénault-Brunet |first4=V. |last5=Massa |first5=D. |last6=Taylor |first6=W.D.|last7=Howarth|first7=I.D. |last8=Sana |first8=H. |last9=Lennon |first9=D.J. |last10=van Loon |first10=J Th. |display-authors=6 |date=1 June 2010 |title=A massive runaway star from 30 Doradus |journal=The Astrophysical Journal|volume=715|issue=2|pages=L74–L79|arxiv=1004.5402|bibcode=2010ApJ...715L..74E|doi=10.1088/2041-8205/715/2/L74|issn=2041-8205|s2cid=118498849}}</ref><ref name="zacharias">{{저널 인용|last1=Zacharias |first1=N. |last2=Finch |first2=C.T. |last3=Girard |first3=T.M. |last4=Henden |first4=A. |last5=Bartlett |first5=J.L.|author5-link=Jennifer Bartlett (astronomer) |last6=Monet|first6=D.G.|last7=Zacharias |first7=M.I. |date=July 2012 |title=VizieR On-Line Data Catalog: UCAC4 Catalogue|journal=VizieR On-Line Data Catalog: I/322A. Originally Published in: 2012yCat.1322....0Z; 2013AJ....145...44Z|volume=1322|bibcode=2012yCat.1322....0Z|s2cid=211646126}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[R136|R136a7]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|127
|163,000
|13.97
|54,000
|항성진화 모델
|{{SIMBAD link|RMC136a7|SIMBAD}}
|<ref name="Brands2022">{{저널 인용|last1=Brands |first1=S. |last2=de Koter |first2=A. |last3=Bestenlehner |first3=J. |last4=Crowther |first4=P. |last5=Sundqvist |first5=J. |last6=Puls |first6=J. |last7=Caballero-Nieves |first7=S. |last8=Abdul-Masih |first8=M. |last9=Driessen |first9=F. |last10=Garcia |first10=M. |last11=Geen |first11=S. |display-authors=6 |date=7 April 2022 |title=The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds |url=https://www.aanda.org/10.1051/0004-6361/202142742 |journal=Astronomy & Astrophysics |arxiv=2202.11080 |bibcode=2022A&A...663A..36B |doi=10.1051/0004-6361/202142742 |issn=0004-6361 |last12=Gräfener |first12=G. |last13=Hawcroft |first13=C. |last14=Kaper |first14=L. |last15=Keszthelyi |first15=Z. |last16=Langer |first16=N. |last17=Sana |first17=H. |last18=Schneider |first18=Fabian R. N. |last19=Shenar |first19=T. |last20=Vink |first20=Jorick S. |volume=663 |page=A36 |s2cid=247025548}}</ref><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[WR 42e]] ([[NGC 3603]]의 [[HD 97950]]에 존재)
|123
|25,000
|14.53
|43,000
|계 이탈
|{{SIMBAD link|WR+42e|SIMBAD}}
|<ref name=soar>{{저널 인용|last1=Roman-Lopes |first1=A. |last2=Franco|first2=G.A.P. |last3=Sanmartim |first3=D. |date=26 May 2016 |title=SOAR Optical and Near-infrared Spectroscopic Survey of Newly Discovered Massive Stars in the Periphery of Galactic Massive Star Clusters I-NGC 3603|journal=The Astrophysical Journal |volume=823 |issue=2 |page=96 |arxiv=1604.01096 |bibcode=2016ApJ...823...96R |doi=10.3847/0004-637X/823/2/96 |issn=1538-4357 |s2cid=119204619 |doi-access=free }}</ref>{{efn|이 특이한 방식의 측정값은 NGC 3603 내 천체 3개가 상호작용하던 중 이 항성이 계를 이탈했다는 가정하에 나온 것이다. 이 항성은 천체 3개 중 근접쌍성 두 개가 하나로 합쳐진 것이다. 이 값은 이론상 비슷한 질량의 항성이 진화과정을 겪었다고 가정했을 때의 잔여질량과 일치한다.}}
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[NGC 3603-A1|HD 97950 A1a]] ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43a A)
|120
|24,800
|11.18<br/>{{small|(연성계 전체)}}
|42,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|Cl*+NGC+3603+BLW+A1|SIMBAD}}
|<ref name="crowther" /><ref name="melena2008" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[LSS 4067]] ([[HM 1]]에 존재)
|120
|11,000
|11.44
|40,000
|항성진화 모델
|{{SIMBAD link|LSS+4067|SIMBAD}}
|<ref name=Massey2001>{{저널 인용|last1=Massey |first1=Philip |last2=DeGioia-Eastwood |first2=Kathleen|author2-link=Kathy Eastwood |last3=Waterhouse |first3=Elizabeth |date=February 2001 |title=The progenitor masses of Wolf-Rayet stars and luminous blue variables determined from cluster turnoffs. II. Results from 12&nbsp;galactic clusters and OB associations |journal=The Astronomical Journal |volume=121 |issue=2 |pages=1050–1070 |arxiv=astro-ph/0010654 |bibcode=2001AJ....121.1050M |doi=10.1086/318769 |issn=0004-6256 |s2cid=53345173}}</ref><ref name="Vazquez">{{저널 인용|last1=Vázquez |first1=R.A. |last2=Baume |first2=G. |date=June 2001 |title=The open cluster Havlen-Moffat no.&nbsp;1 revisited |journal=Astronomy & Astrophysics |volume=371 |issue=3 |pages=908–920 |bibcode=2001A&A...371..908V |doi=10.1051/0004-6361:20010410 |issn=0004-6361 |s2cid=121918776|doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[피스미스 24|WR 93]] ([[NGC 6357]]의 [[피스미스 24]]에 존재)
|120
|5,900
|10.68
|71,000
|항성진화 모델
|{{SIMBAD link|WR+93|SIMBAD}}
|<ref name=Massey2001/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[Sk -69° 212]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|119
|160,000
|12.416
|45,400
|항성진화 모델
|{{SIMBAD link|Sk+-69+212|SIMBAD}}
|<ref name=Massey2000>{{저널 인용|last1=Massey|first1=Philip |last2=Waterhouse |first2=Elizabeth |last3=DeGioia-Eastwood |first3=Kathleen |author3-link=Kathy Eastwood|date=May 2000 |title=The progenitor masses of Wolf-Rayet stars and luminous blue variables determined from cluster turnoffs. I. Results from 19&nbsp;OB&nbsp;associations in the Magellanic Clouds |journal=The Astronomical Journal |volume=119 |issue=5 |pages=2214–2241 |arxiv=astro-ph/0002233 |bibcode=2000AJ....119.2214M |doi=10.1086/301345 |issn=0004-6256 |s2cid=16891188}}</ref><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[Sk -69° 249]] A ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
|119
|160,000
|12.02<br/>{{small|(연성계 전체)}}
|38,900
|항성진화 모델
|{{SIMBAD link|Sk+-69+249|SIMBAD}}
|<ref name=Massey2000/><ref name=Tycho2>{{저널 인용|last1=Fabricius |first1=C. |last2=Høg |first2=E. |last3=Makarov |first3=V.V. |last4=Mason |first4=B.D. |last5=Wycoff |first5=G.L. |last6=Urban |first6=S.E. |date=March 2002 |title=The Tycho double star catalogue |journal=Astronomy & Astrophysics |volume=384|issue=1|pages=180–189 |bibcode=2002A&A...384..180F |doi=10.1051/0004-6361:20011822 |issn=0004-6361 |s2cid=56060737|doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[ST5-31]] ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
|119
|160,000
|12.273
|50,700
|항성진화 모델
|{{SIMBAD link|ST92+5-31|SIMBAD}}
|<ref name=Massey2000/><ref name=Zaritsky>{{저널 인용|last1=Zaritsky |first1=Dennis |last2=Harris |first2=Jason |last3=Thompson |first3=Ian B. |last4=Grebel |first4=Eva K. |date=October 2004 |title=The Magellanic Clouds Photometric Survey: The Large Magellanic Cloud Stellar Catalog and Extinction Map |journal=The Astronomical Journal |language=en |volume=128 |issue=4 |pages=1606–1614 |arxiv=astro-ph/0407006 |bibcode=2004AJ....128.1606Z |doi=10.1086/423910 |issn=0004-6256 |s2cid=119532934}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[R136|R136a5]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|116
|157,000
|13.71
|48,000
|항성진화 모델
|{{SIMBAD link|RMC136a5|SIMBAD}}
|<ref name="Brands2022" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[MSP 183]] ([[웨스터룬드 2]]에 존재)
|115
|20,000
|13.878
|46,300
|분광법
|{{SIMBAD link|Cl*+Westerlund+2+MSP+183|SIMBAD}}
|<ref>{{저널 인용|last1=Drew |first1=J.E. |last2=Herrero |first2=A. |last3=Mohr-Smith |first3=M. |last4=Monguió |first4=M. |last5=Wright |first5=N.J. |last6=Kupfer |first6=T. |last7=Napiwotzki |first7=R. |date=21 October 2018 |title=Massive stars in the hinterland of the young cluster, Westerlund&nbsp;2 |journal=Monthly Notices of the Royal Astronomical Society |lang=en |volume=480 |issue=2 |pages=2109–2124 |arxiv=1807.06486 |bibcode=2018MNRAS.480.2109D |doi=10.1093/mnras/sty1905 |issn=0035-8711 |s2cid=53126230}}</ref><ref>{{저널 인용|last1=Vargas Álvarez |first1=Carlos A. |last2=Kobulnicky |first2=Henry A. |last3=Bradley |first3=David R. |last4=Kannappan |first4=Sheila J. |last5=Norris |first5=Mark A. |last6=Cool |first6=Richard J. |last7=Miller |first7=Brendan P. |date=25 March 2013 |title=The distance to the massive galactic cluster Westerlund&nbsp;2 from a spectroscopic and HST photometric study |journal=The Astronomical Journal |volume=145 |issue=5 |page=125 |arxiv=1302.0863 |bibcode=2013AJ....145..125V |doi=10.1088/0004-6256/145/5/125 |issn=0004-6256|s2cid=67769122}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[WR 24]] ([[용골자리 성운]]의 [[콜린더 228]]에 존재)
|114
|14,000
| style="background:lightblue;color:darkblue;" |'''6.48'''
|50,100
|항성진화 모델
|{{SIMBAD link|WR+24|SIMBAD}}
|<ref name="hamann2019">{{저널 인용|last1=Hamann |first1=W.-R. |last2=Gräfener |first2=G. |last3=Liermann |first3=A. |last4=Hainich |first4=R. |last5=Sander |first5=A.a.C. |last6=Shenar |first6=T. |last7=Ramachandran |first7=V. |last8=Todt |first8=H. |last9=Oskinova |first9=L.M. |display-authors=6 |date=1 May 2019 |title=The galactic WN&nbsp;stars revisited - impact of Gaia distances on fundamental stellar parameters |journal=Astronomy & Astrophysics |language=en |volume=625 |page=A57 |arxiv=1904.04687 |bibcode=2019A&A...625A..57H |doi=10.1051/0004-6361/201834850|issn=0004-6361|s2cid=104292503}}</ref><ref name="gcvs">{{저널 인용|last1=Samus |first1=N.N. |last2=Kazarovets |first2=E.V. |last3=Durlevich |first3=O.V. |last4=Kireeva |first4=N.N. |last5=Pastukhova |first5=E.N. |date=January 2009 |title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013) |journal=VizieR On-Line Data Catalog: B/GCVS. Originally Published in: 2017ARep...61...80S; 2017AZh....94...87S |volume=1 |bibcode=2009yCat....102025S |s2cid=208116145}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[NGC 3603-C|HD 97950 C]]1 ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43c A)
|113
|24,800
|11.89<br/>{{small|(연성계 전체)}}
|44,000
|분광법
|{{SIMBAD link|HD+97950C|SIMBAD}}
|<ref name=crowther/><ref name=melena2008/><ref group="lower-alpha" name="Binary">쌍성계지만 동반성이 주성에 비해 매우 가볍다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[아치스 성단|아치스]]-F9 ([[아치스 성단]]에 존재하는 WR 102ae)
|111.3
|25,000
|16.1<br/>{{small|(J&nbsp;대역)}}
|36,600
|분광법
|{{SIMBAD link|FNG2002+9|SIMBAD}}
|<ref name="grafener">{{저널 인용|last1=Gräfener |first1=G. |last2=Vink |first2=J.S. |last3=de&nbsp;Koter |first3=A. |last4=Langer |first4=N. |date=November 2011 |title=The Eddington factor as the key to understand the winds of the most massive stars: Evidence for a Γ-dependence of Wolf-Rayet type mass loss |journal=Astronomy & Astrophysics |volume=535 |page=A56 |arxiv=1106.5361 |bibcode=2011A&A...535A..56G |doi=10.1051/0004-6361/201116701 |issn=0004-6361 |s2cid=59396651}}</ref><ref name=Figer>{{저널 인용|last1=Figer|first1=Donald F.|last2=Najarro|first2=Francisco|last3=Gilmore|first3=Diane|last4=Morris|first4=Mark|last5=Kim|first5=Sungsoo S.|last6=Serabyn|first6=Eugene|last7=McLean|first7=Ian S.|last8=Gilbert|first8=Andrea M.|last9=Graham|first9=James R.|last10=Larkin|first10=James E.|last11=Levenson|first11=N.A. |display-authors=6 |date=10 December 2002|title=Massive Stars in the Arches Cluster|journal=The Astrophysical Journal|language=en|volume=581|issue=1|pages=258–275|arxiv=astro-ph/0208145|bibcode=2002ApJ...581..258F|doi=10.1086/344154|issn=0004-637X|s2cid=119002004|last12=Harry I.|first12=Teplitz}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" |[[백조자리 OB2-12|백조자리 OB2 #12]] A ([[백조자리 OB2]]에 존재)
|110
|5,200
|11.702<br/>{{small|(연성계 전체)}}
|13,700
|분광법
|{{SIMBAD link|Cyg+OB2+12|SIMBAD}}
|<ref name="clark">{{저널 인용|last1=Clark|first1=J. S.|last2=Najarro|first2=F.|last3=Negueruela|first3=I.|last4=Ritchie|first4=B. W.|last5=Urbaneja|first5=M. A.|last6=Howarth|first6=I. D.|date=May 2012|title=On the nature of the galactic early-B hypergiants|journal=Astronomy & Astrophysics|volume=541|page=A145|arxiv=1202.3991|bibcode=2012A&A...541A.145C|doi=10.1051/0004-6361/201117472|issn=0004-6361|s2cid=11978733}}</ref><ref name=Laur>{{저널 인용|last1=Laur|first1=Jaan|last2=Kolka|first2=Indrek|last3=Eenmäe|first3=Tõnis|last4=Tuvikene|first4=Taavi|last5=Leedjärv|first5=Laurits|date=February 2017|title=Variability survey of brightest stars in selected OB associations|journal=Astronomy & Astrophysics|volume=598|page=A108|arxiv=1611.02452|bibcode=2017A&A...598A.108L|doi=10.1051/0004-6361/201629395|issn=0004-6361|s2cid=119076598}}</ref><ref group=lower-alpha name=Binary/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[HD 93129]] Aa ([[용골자리 성운]]의 [[트럼플러 14]]에 존재)
|110
|7,500
|6.9<br/>{{small|(연성계 전체)}}
|42,500
|케플러의 법칙<br>(삼중성)
|{{SIMBAD link|HD+93129A|SIMBAD}}
|<ref name=nelan>{{저널 인용|last1=Nelan |first1=Edmund P. |last2=Walborn |first2=Nolan R. |last3=Wallace |first3=Debra J. |last4=Moffat |first4=Anthony F.J. |last5=Makidon |first5=Russell B. |last6=Gies |first6=Douglas R. |last7=Panagia |first7=Nino |date=July 2004 |title=Resolving OB systems in the Carina nebula with the Hubble Space Telescope Fine Guidance Sensor |journal=The Astronomical Journal |language=en |volume=128 |issue=1 |pages=323–329 |bibcode=2004AJ....128..323N |doi=10.1086/420716 |issn=0004-6256 |s2cid=121115585|doi-access=free }}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-36]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|110
|163,000
|14.41
|49,500
|항성진화 모델
|{{SIMBAD link|HSH95+36|SIMBAD}}
|<ref name="Brands2022" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[R146]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|109
|164,000
|13.11
|63,000
|분광법
|{{SIMBAD link|RMC146|SIMBAD}}
|<ref name="hainich"/><ref name="Doran2013"/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[R136|R136a4]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|108
|157,000
|13.41
|50,000
|항성진화 모델
|{{SIMBAD link|RMC136a4|SIMBAD}}
|<ref name="Brands2022" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 621]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|107
|164,000
|15.39
|54,000
|분광법
|{{SIMBAD link|VFTS+621|SIMBAD}}
|<ref name="best"/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[R136|R136a6]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|105
|157,000
|13.35
|52,000
|항성진화 모델
|{{SIMBAD link|RMC136a6|SIMBAD}}
|<ref name="Brands2022" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[웨스터하우트 49]]-3 ([[웨스터하우트 49]]에 존재)
|105
|36,200
|16.689<br/>{{small|(J&nbsp;대역)}}
|40,700
|항성진화 모델
|{{SIMBAD link|WBB2016+3|SIMBAD}}
|<ref name=Wu2016/><ref name=2MASS/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 21a]] A ([[웨스터룬드 2]]에 존재하는 [[폭주성]])
|103.6
|26,100
|12.661 {{small|(연성계 전체)}}
|45,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|WR+21a|SIMBAD}}
|<ref name=tramper>{{저널 인용|last1=Tramper |first1=F. |last2=Sana |first2=H. |last3=Fitzsimons |first3=N.E. |last4=de Koter |first4=A. |last5=Kaper |first5=L. |last6=Mahy |first6=L. |last7=Moffat |first7=A. |date=11 January 2016 |title=The mass of the very massive binary WR21a |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=455 |issue=2 |pages=1275–1281 |arxiv=1510.03609 |bibcode=2016MNRAS.455.1275T |doi=10.1093/mnras/stv2373 |issn=0035-8711 |s2cid=44364798}}</ref><ref name="zacharias" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[R99]] ([[대마젤란 은하]]의 [[N44 (방출 성운)|N44]]에 존재)
|103
|164,000
|11.52
|28,000
|분광법
|{{SIMBAD link|RMC99|SIMBAD}}
|<ref name=hainich/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[아치스 성단|아치스]]-F6 ([[아치스 성단]]에 존재하는 WR 102ah)
|101
|25,000
|15.75<br/>{{small|(J&nbsp;대역)}}
|33,900
|분광법
|{{SIMBAD link|FNG2002+6|SIMBAD}}
|<ref name="grafener" /><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -65° 47]] ([[대마젤란 은하]]의 [[NGC 1923]]에 존재)
|101
|160,000
|12.466
|47,800
|항성진화 모델
|{{SIMBAD link|Sk+-65+47|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" |[[아치스 성단|아치스]]-F1 ([[아치스 성단]]에 존재하는 WR 102ad)
|100.9
|25,000
|16.3<br/>{{small|(J&nbsp;대역)}}
|33,200
|분광법
|{{SIMBAD link|FNG2002+1|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[WR 102ka|작약성운 별]] ([[은하중심]] 근처의 [[작약성운]]에 존재하는 WR 102ka)
|100
|26,000
|12.978<br/>{{small|(J&nbsp;대역)}}
|25,100
|분광법
|{{SIMBAD link|Peony+Star|SIMBAD}}
|<ref name="oskinova">{{저널 인용|last1=Oskinova|first1=L. M.|last2=Steinke|first2=M.|last3=Hamann|first3=W.-R.|last4=Sander|first4=A.|last5=Todt|first5=H.|last6=Liermann|first6=A.|date=21 December 2013|title=One of the most massive stars in the Galaxy may have formed in isolation|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=436|issue=4|pages=3357–3365|arxiv=1309.7651|bibcode=2013MNRAS.436.3357O|doi=10.1093/mnras/stt1817|issn=0035-8711|s2cid=118513968}}</ref><ref name=2MASS/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[VFTS 457]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|100
|164,000
|13.74
|39,800
|분광법
|{{SIMBAD link|VFTS+457|SIMBAD}}
|<ref name="best"/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[용골자리 에타]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|100
|7,500
| style="background:lightblue;color:darkblue;" | '''4.3'''<br/>{{small|(연성계 전체)}}
|9,400–35,200
|분광법
|{{SIMBAD link|Eta+Carinae|SIMBAD}}
|<ref name="clementel">{{저널 인용|last1=Clementel |first1=N. |last2=Madura |first2=T.I. |last3=Kruip |first3=C.J.H. |last4=Paardekooper |first4=J.-P. |last5=Gull |first5=T.R. |date=1 March 2015 |title=3D radiative transfer simulations of Eta Carinae's inner colliding winds - I. Ionization structure of helium at apastron |journal=Monthly Notices of the Royal Astronomical Society |lang=en |volume=447 |issue=3 |pages=2445–2458 |arxiv=1412.7569 |bibcode=2015MNRAS.447.2445C|doi=10.1093/mnras/stu2614 |issn=0035-8711 |s2cid=118405692}}</ref><ref name="2018-07-02_NAL">{{저널 인용|last1=Hamaguchi |first1=Kenji |last2=Corcoran |first2=Michael F. |last3=Pittard |first3=Julian M. |last4=Sharma |first4=Neetika |last5=Takahashi|first5=Hiromitsu|last6=Russell|first6=Christopher M.P. |last7=Grefenstette |first7=Brian W.|last8=Wik |first8=Daniel R.|last9=Gull |first9=Theodore R. |last10=Richardson |first10=Noel D. |last11=Madura |first11=Thomas I. |first12=Anthony F.J. |last12=Moffat |display-authors=6 |date=September 2018 |title=Non-thermal X-rays from colliding wind shock acceleration in the massive binary Eta Carinae |journal=Nature Astronomy |lang=en |volume=2 |issue=9 |pages=731–736 |arxiv=1904.09219 |bibcode=2018NatAs...2..731H |doi=10.1038/s41550-018-0505-1 |issn=2397-3366 |s2cid=126188024}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[머서 30]]-1 A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-3 A)
|99
|40,000
|10.33<br/>{{small|(J&nbsp;대역)}}
|32,200
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-1|SIMBAD}}
|<ref name=Fuente>{{저널 인용|last1=de la Fuente |first1=D. |last2=Najarro |first2=F. |last3=Borissova |first3=J. |last4=Ramírez Alegría |first4=S. |last5=Hanson |first5=M.M. |last6=Trombley |first6=C. |last7=Figer |first7=D.F. |last8=Davies |first8=B. |last9=Garcia |first9=M. |last10=Kurtev|first10=R. |last11=Urbaneja |first11=M.A. |last12=Smith |first12=L.C. |last13=Lucas |first13=P.W. |last14=Herrero |first14=A. |display-authors=6 |date=May 2016 |title=Probing the Dragonfish star-forming complex: The ionizing population of the young massive cluster Mercer&nbsp;30 |journal=Astronomy & Astrophysics |volume=589 |page=A69 |arxiv=1602.02503 |bibcode=2016A&A...589A..69D |doi=10.1051/0004-6361/201528004 |issn=0004-6361 |s2cid=119096455}}</ref><ref group="lower-alpha" name=Mc30>머서 30은 드래곤피쉬 성운의 산개성단이다.</ref><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -68° 137]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|99
|160,000
|13.346
|50,000
|분광법
|{{SIMBAD link|Sk+-68+137|SIMBAD}}
|<ref name="fulltext" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 25]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|98
|6,500
|8.8<br/>{{small|(연성계 전체)}}
|50,100
|항성진화 모델
|{{SIMBAD link|WR+25|SIMBAD}}
|<ref name=hamann2019/><ref name=ducati/><ref group=lower-alpha name=Binary/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[BI 253]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재하는 [[폭주성]])
|97.6
|164,000
|13.76
|54,000
|분광법
|{{SIMBAD link|BI+253|SIMBAD}}
|<ref name="schneider2018" /><ref>{{저널 인용|last1=Rivero González |first1=J.G. |last2=Puls |first2=J. |last3=Najarro |first3=F. |last4=Brott |first4=I. |date=January 2012 |title=Nitrogen line spectroscopy of O-stars: II. Surface nitrogen abundances for O-stars in the Large Magellanic Cloud |journal=Astronomy & Astrophysics |volume=537 |page=A79 |arxiv=1110.5148 |bibcode=2012A&A...537A..79R |doi=10.1051/0004-6361/201117790 |issn=0004-6361 |s2cid=119110554}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[R136|R136a8]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|96
|157,000
|14.42
|49,500
|항성진화 모델
|{{SIMBAD link|RMC136a8|SIMBAD}}
|<ref name="Brands2022" /><ref name=crowther2016>{{저널 인용|last1=Crowther |first1=Paul A. |last2=Caballero-Nieves |first2=S.M. |last3=Bostroem |first3=K.A. |last4=Apellániz |first4=J. Maíz |last5=Schneider |first5=F.R.N. |last6=Walborn |first6=N.R. |last7=Angus |first7=C.R. |last8=Brott |first8=I. |last9=Bonanos |first9=A. |last10=de Koter |first10=A. |last11=de Mink |first11=S.E. |display-authors=6 |date=1 May 2016 |title=The R136 star cluster dissected with Hubble Space Telescope / STIS. I. Far-ultraviolet spectroscopic census and the origin of He{{sup{{sc|ii}}}} λ1640 in young star clusters |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=458 |issue=1 |pages=624–659 |arxiv=1603.04994 |bibcode=2016MNRAS.458..624C |doi=10.1093/mnras/stw273 |issn=0035-8711 |last12=Evans |first12=C.J. |last13=Gräfener |first13=G. |last14=Herrero |first14=A. |last15=Howarth |first15=I.D. |last16=Langer |first16=N. |last17=Lennon |first17=D.J. |last18=Puls |first18=J. |last19=Sana |first19=H. |last20=Vink |first20=J.S. |s2cid=119131482}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[HD 38282]] B ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|95
|163,000
|11.11<br/>{{small|(연성계 전체)}}
|47,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|HD+38282|SIMBAD}}
|<ref name="sana">{{저널 인용|last1=Sana |first1=H. |last2=van Boeckel |first2=T. |last3=Tramper |first3=F. |last4=Ellerbroek |first4=L. E.|last5=de Koter |first5=A. |last6=Kaper |first6=L. |last7=Moffat|first7=A.F.J. |last8=Schnurr |first8=O. |last9=Schneider |first9=F.R.N. |last10=Gies |first10=D.R. |display-authors=6 |date=15 March 2013|title=R144 revealed as a double-lined spectroscopic binary|journal=Monthly Notices of the Royal Astronomical Society: Letters|language=en|volume=432|issue=1|pages=L26–L30|arxiv=1304.4591|bibcode=2013MNRAS.432L..26S|doi=10.1093/mnrasl/slt029|issn=1745-3933|s2cid=119238483}}</ref><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HM 1]]-6 ([[HM 1]]에 존재)
|95
|11,000
|11.64
|44,700
|항성진화 모델
|{{SIMBAD link|Cl+HM+1+6|SIMBAD}}
|<ref name=Massey2001/><ref name=Reed>{{저널 인용|last=Reed|first=B. Cameron|date=May 2003|title=Catalog of Galactic OB Stars|journal=The Astronomical Journal|language=en|volume=125|issue=5|pages=2531–2533|bibcode=2003AJ....125.2531R|doi=10.1086/374771|issn=0004-6256|s2cid=121285799|doi-access=free}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 97950|NGC 3603]]-42 ([[NGC 3603]]의 [[HD 97950]]에 존재)
|95
|25,000
|12.86
|50,000
|분광법
|{{SIMBAD link|Cl*+NGC+3603+MDS+42|SIMBAD}}
|<ref name="fulltext" /><ref name=melena2008/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[R139]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|95
|163,000
|11.94<br/>{{small|(연성계 전체)}}
|35,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|RMC139|SIMBAD}}
|<ref name="hainich" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-6]] ([[대마젤란 은하]]의 [[NGC 1747]]에 존재)
|94
|165,000
|11.95
|56,000
|분광법
|{{SIMBAD link|BAT99+6|SIMBAD}}
|<ref name="hainich" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[Sk -66° 172]] ([[대마젤란 은하]]의 [[N64 (성운)|N64]]에 존재)
|94
|160,000
|13.1
|46,300
|분광법
|{{SIMBAD link|Sk+-66+172|SIMBAD}}
|<ref name="fulltext" /><ref name=Bonanos/><ref group="lower-alpha">N64은 대마젤란 은하의 방출성운이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[ST2-22]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|94
|160,000
|14.3
|51,300
|항성진화 모델
|{{SIMBAD link|ST92+2-22|SIMBAD}}
|<ref name=Massey2000/><ref name=Schild>{{저널 인용|last1=Schild |first1=H. |last2=Testor |first2=G. |date=March 1992 |title=Spectral types and UBV magnitudes of stars in the 30 Doradus complex |journal=Astronomy and Astrophysics Supplement Series |volume=92 |pages=729–748 |bibcode=1992A&AS...92..729S |issn=0365-0138 |s2cid=115371295}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" |[[VFTS 259]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|94
|164,000
|13.65
|37,600
|분광법
|{{SIMBAD link|VFTS+259|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 562]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|94
|164,000
|13.66
|42,200
|분광법
|{{SIMBAD link|VFTS+562|SIMBAD}}
|<ref name="best" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 512]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|93
|164,000
|14.28
|47,300
|분광법
|{{SIMBAD link|VFTS+512|SIMBAD}}
|<ref name="best" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[NGC 3603-A1|HD 97950 A1b]] ([[NGC 3603]]의 [[HD 97950]]에 존재하는 WR 43a B)
|92
|24,800
|11.18<br/>{{small|(연성계 전체)}}
|40,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|Cl*+NGC+3603+BLW+A1|SIMBAD}}
|<ref name="crowther" /><ref name=melena2008/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[R136b]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|92
|163,000
|13.24
|35,500
|항성진화 모델
|{{SIMBAD link|RMC136b|SIMBAD}}
|<ref name="Brands2022" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 16]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|91.6
|164,000
|13.55
|50,600
|분광법
|{{SIMBAD link|VFTS+16|SIMBAD}}
|<ref name="schneider2018" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 97950]] A3 ([[NGC 3603]]의 [[HD 97950]]에 존재)
|91
|24,800
|12.95
|50,000
|분광법
|{{SIMBAD link|Cl*+NGC+3603+BLW+A3|SIMBAD}}
|<ref name="fulltext" /><ref name=melena2008/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[NGC 346]]-W1 ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|91
|200,000
|12.57
|43,400
|항성진화 모델
|{{SIMBAD link|Cl*+NGC+346+W+1|SIMBAD}}
|<ref name=Massey2000/><ref name=spitzer>{{저널 인용|last1=Bonanos |first1=A.Z. |last2=Lennon |first2=D.J. |last3=Köhlinger |first3=F. |last4=van Loon |first4=J.Th. |last5=Massa |first5=D. L. |last6=Sewilo |first6=M. |last7=Evans|first7=C.J. |last8=Panagia |first8=N. |last9=Babler |first9=B.L. |last10=Block |first10=M. |last11=Bracker |first11=S. |last12=Engelbracht |first12=C.W. |last13=Gordon |first13=K.D. |last14=Hora |first14=J.L. |last15=Indebetouw |first15=R. |last16=Meade |first16=M.R. |last17=Meixner |first17=M.|last18=Misselt |first18=K.A. |last19=Robitaille |first19=T.P. |last20=Shiao |first20=B. |last21=Whitney |first21=B.A. |display-authors=6 |date=1 August 2010 |title=Spitzer SAGE-SMC infrared photometry of massive stars in the Small Magellanic Cloud |journal=[[The Astronomical Journal]] |volume=140 |issue=2 |pages=416–429 |arxiv=1004.0949 |bibcode=2010AJ....140..416B |doi=10.1088/0004-6256/140/2/416 |hdl=1887/61635 |issn=0004-6256 |s2cid=119290443}}</ref>
|- style="text-align:center;"
| style="background:{{항성-색깔|O}};text-align:left;" |[[웨스터하우트 49-2]] ([[웨스터하우트 49]]에 존재)
| 90–240, {{val|250|120}}
|36,200
|18.246<br/>{{small|(J&nbsp;대역)}}
|35,500
|분광법
|{{SIMBAD link|WBB2016+2|SIMBAD}}
|<ref name=Wu2016>{{저널 인용|last1=Wu |first1=Shi-Wei |last2=Bik |first2=Arjan |last3=Bestenlehner |first3=Joachim M. |last4=Henning |first4=Thomas |last5=Pasquali |first5=Anna |last6=Brandner |first6=Wolfgang |last7=Stolte |first7=Andrea |date=May 2016 |title=The massive stellar population of W49: A spectroscopic survey|journal=Astronomy & Astrophysics |volume=589 |page=A16 |arxiv=1602.05190 |bibcode=2016A&A...589A..16W|doi=10.1051/0004-6361/201527823|issn=0004-6361|s2cid=59425112}}</ref><ref name=2MASS>{{보고서 인용|last1=Cutri |first1=Roc M. |last2=Skrutskie |first2=Michael F. |last3=van&nbsp;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.  |display-authors=6 |year=2003 |title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) |publisher=CDS/ADC |series=Collection of Electronic Catalogues |bibcode=2003yCat.2246....0C |page=II/246 |volume=2246 |url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246 |s2cid=115529446}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[R127]] ([[대마젤란 은하]]의 [[NGC 2055]]에 존재)
|90
|160,000
|10.15
|10,000–27,000
|항성진화 모델
|{{SIMBAD link|RMC127|SIMBAD}}
|<ref name=Smith2015>{{저널 인용|last1=Smith |first1=Nathan |last2=Tombleson |first2=Ryan |date=11 February 2015 |title=Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution |journal=[[Monthly Notices of the Royal Astronomical Society]] |lang=en |volume=447 |issue=1 |pages=598–617 |arxiv=1406.7431 |bibcode=2015MNRAS.447..598S |doi=10.1093/mnras/stu2430 |issn=1365-2966 |s2cid=119284620}}</ref><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 333]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|90
|164,000
|12.49
|37,600
|분광법
|{{SIMBAD link|VFTS+333|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 267]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|89
|164,000
|13.49
|44,700
|분광법
|{{SIMBAD link|VFTS+267|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 64]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|88
|164,000
|14.621
|39,800
|분광법
|{{SIMBAD link|VFTS+64|SIMBAD}}
|<ref name=best/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-80]] A ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|87
|165,000
|13<br/>{{small|(연성계 전체)}}
|45,000
|분광법
|{{SIMBAD link|BAT99+80|SIMBAD}}
|<ref name=Massey2000/><ref name=Schild/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[R140b]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|87
|165,000
|12.66
|47,000
|분광법
|{{SIMBAD link|RMC140b|SIMBAD}}
|<ref name=hainich/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[VFTS 542]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|87
|164,000
|13.47
|44,700
|분광법
|{{SIMBAD link|VFTS+542|SIMBAD}}
|<ref name="best" /><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 599]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|87
|164,000
|13.8
|44,700
|분광법
|{{SIMBAD link|VFTS+599|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 89]] ([[HM 1]]에 존재)
|87
|11,000
|11.02
|39,800
|항성진화 모델
|{{SIMBAD link|WR+89|SIMBAD}}
|<ref name=hamann2019/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[아치스 성단|아치스]]-F7 ([[아치스 성단]]에 존재하는 WR 102aj)
|86.3
|25,000
|15.74<br/>{{small|(J&nbsp;대역)}}
|32,900
|분광법
|{{SIMBAD link|FNG2002+7|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -69° 104]] ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|86
|160,000
|12.1
|39,900
|항성진화 모델
|{{SIMBAD link|Sk+-69+104|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[VFTS 1017]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|86
|164,000
|14.5
|50,100
|분광법
|{{SIMBAD link|VFTS+1017|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 10]]-3061 ([[대마젤란 은하]]의 [[NGC 1763]]에 존재)
|85
|160,000
|13.491
|52,000
|분광법
|{{SIMBAD link|L72+LH+10-3061|SIMBAD}}
|<ref name="fulltext" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[NGC 346|Sk 80]] ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|85
|200,000
|12.31
|38,900
|항성진화 모델
|{{SIMBAD link|Sk+80|SIMBAD}}
|<ref name=Massey2000/><ref>{{저널 인용|last1=Evans |first1=C.J. |last2=Lennon |first2=D.J. |last3=Smartt |first3=S. J. |last4=Trundle |first4=C. |date=September 2006 |title=The VLT-FLAMES survey of massive stars: observations centered on the Magellanic Cloud clusters NGC 330, NGC 346, NGC 2004, and the N11 region |journal=[[Astronomy & Astrophysics]] |volume=456 |issue=2 |pages=623–638 |arxiv=astro-ph/0606405 |bibcode=2006A&A...456..623E |doi=10.1051/0004-6361:20064988 |issn=0004-6361 |s2cid=13160849}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 603]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|85
|164,000
|13.99
|42,200
|분광법
|{{SIMBAD link|VFTS+603|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -70° 91]] ([[대마젤란 은하]]의 [[BSDL 1830]]에 존재)
|84.09
|165,000
|12.78
|48,900
|항성진화 모델
|{{SIMBAD link|Sk+-70+91|SIMBAD}}
|<ref name=Massa2017>{{저널 인용|last1=Massa|first1=D.|last2=Fullerton|first2=A. W.|last3=Prinja|first3=R. K.|date=September 2017|title=Mass-loss rates from mid-infrared excesses in LMC and SMC O stars|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=470|issue=3|pages=3765–3774|arxiv=1706.02627|bibcode=2017MNRAS.470.3765M|doi=10.1093/mnras/stx1443|issn=0035-8711|s2cid=119475951}}</ref><ref name=Bonanos/><ref group="lower-alpha">BSDL 1830은 대마젤란 은하의 성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[R147]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|84
|164,000
|12.993
|47,300
|분광법
|{{SIMBAD link|RMC147|SIMBAD}}
|<ref name=best/><ref name=Ulaczyk/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 93250]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|83.3
|7,500
|7.5<br/>{{small|(연성계 전체)}}
|46,000
|항성진화 모델
|{{SIMBAD link|HD+93250|SIMBAD}}
|<ref name=weidner>{{저널 인용|last1=Weidner |first1=C. |last2=Vink |first2=J.S. |date=December 2010 |title=The masses, and the mass discrepancy of O-type stars |journal=[[Astronomy & Astrophysics]] |volume=524 |page=A98 |arxiv=1010.2204 |bibcode=2010A&A...524A..98W |doi=10.1051/0004-6361/201014491 |issn=0004-6361 |s2cid=118836634}}</ref><ref name=ducati/><ref group=lower-alpha name=Binary/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[멜닉 33Na]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|83
|163,000
|13.79<br/>{{small|(연성계 전체)}}
|50,000
|항성진화 모델
|{{SIMBAD link|Cl*+NGC+2070+MEL+33N|SIMBAD}}
|<ref name=Bestenlehner2022>{{저널 인용|doi=10.1093/mnras/stab3521|title=Melnick 33Na: A very massive colliding-wind binary system in 30 Doradus|year=2022|last1=Bestenlehner|first1=Joachim M.|last2=Crowther|first2=Paul A.|last3=Broos|first3=Patrick S.|last4=Pollock|first4=Andrew M T.|last5=Townsley|first5=Leisa K.|journal=Monthly Notices of the Royal Astronomical Society|volume=510|issue=4|pages=6133–6149|bibcode=2022MNRAS.510.6133B|arxiv=2112.00022}}</ref><ref name=Castro2018>{{저널 인용|doi=10.1051/0004-6361/201732084|title=Mapping the core of the Tarantula Nebula with VLT-MUSE. I. Spectral and nebular content around R136|year=2018 |author1=Castro, N. |author2=Crowther, P. A. |author3=Evans, C.J. |author4=Mackey, J. |author5=Castro-Rodriguez, N. |author6=Vink, J.S. |author7=Melnick, J. |author8=Selman, F. |display-authors=6 |journal=[[Astronomy & Astrophysics]] |volume=614 |id=A147 |page=12 |arxiv=1802.01597 |bibcode=2018A&A...614A.147C |s2cid=119341920}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 20a]] A ([[웨스터룬드 2]]에 존재)
|82.7
|20,000
|13.28<br/>{{small|(연성계 전체)}}
|43,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|WR+20a|SIMBAD}}
|<ref name="rauw">{{저널 인용|last1=Rauw |first1=G. |last2=Crowther |first2=P.A. |last3=de Becker |first3=M. |last4=Gosset |first4=E. |last5=Nazé |first5=Y. |last6=Sana |first6=H. |last7=van der Hucht |first7=K.A. |last8=Vreux |first8=J.-M. |last9=Williams |first9=P.M. |display-authors=6 |date=March 2005 |title=The spectrum of the very massive binary system WR 20a (WN6ha + WN6ha): Fundamental parameters and wind interactions |journal=Astronomy & Astrophysics |volume=432 |issue=3 |pages=985–998 |bibcode=2005A&A...432..985R |doi=10.1051/0004-6361:20042136 |doi-access=free |issn=0004-6361 |s2cid=53372849}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[TIC 276934932]] A ([[대마젤란 은하]]의 [[NGC 2048]]에 존재)
|82
|160,000
|14.05<br/>{{small|(연성계 전체)}}
|45,000
|분광법
|{{SIMBAD link|TIC+276934932|SIMBAD}}
|<ref name="fulltext"/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 20a]] B ([[웨스터룬드 2]]에 존재)
|81.9
|20,000
|13.28<br/>{{small|(연성계 전체)}}
|43,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|WR+20a|SIMBAD}}
|<ref name="rauw" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[트럼플러 27]]-27 ([[트럼플러 27]]에 존재)
|81
|3,900
|13.31
|37,000
|항성진화 모델
|{{SIMBAD link|Cl+Trumpler+27+27|SIMBAD}}
|<ref name=Massey2001/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-96]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|80
|165,000
|13.76
|42,000
|분광법
|{{SIMBAD link|BAT99+96|SIMBAD}}
|<ref name=hainich/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 15570]] ([[하트 성운]]의 [[IC 1805]]에 존재)
|80
|7,500
|8.11
|46,000
|분광법
|{{SIMBAD link|HD+15570|SIMBAD}}
|<ref name=debecker/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[HD 38282]] A ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|80
|163,000
|11.11<br/>{{small|(연성계 전체)}}
|47,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|HD+38282|SIMBAD}}
|<ref name=sana/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-46]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|80
|163,000
|14.56
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+46|SIMBAD}}
|<ref name=Brands2022/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[아치스 성단|아치스]]-F15 ([[아치스 성단]]에 존재)
|79.7
|25,000
|16.12<br/>{{small|(J&nbsp;대역)}}
|35,600
|분광법
|{{SIMBAD link|FNG2002+15|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[BI 237]] ([[대마젤란 은하]]의 [[BSDL 2527]]에 존재)
|79.66
|165,000
|13.83
|51,300
|분광법
|{{SIMBAD link|BI+237|SIMBAD}}
|<ref name=Massa2017/><ref name=Bonanos/><ref group="lower-alpha">BSDL 2527은 대마젤란 은하의 성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 94]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|79
|164,000
|14.161
|42,200
|분광법
|{{SIMBAD link|VFTS+94|SIMBAD}}
|<ref name="best" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 151]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|79
|164,000
|14.13
|42,200
|분광법
|{{SIMBAD link|VFTS+151|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 41]]-32 ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|78
|160,000
|13.086
|48,200
|항성진화 모델
|{{SIMBAD link|L72+LH+41-32|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[피스미스 24]]-17 ([[NGC 6357]]의 [[피스미스 24]]에 존재)
|78
|5,900
|11.84
|42,700
|분광법
|{{SIMBAD link|Cl+Pismis+24+17|SIMBAD}}
|<ref name="fang">{{저널 인용|last1=Fang|first1=M.|last2=van Boekel|first2=R.|last3=King|first3=R. R.|last4=Henning|first4=Th.|last5=Bouwman|first5=J.|last6=Doi|first6=Y.|last7=Okamoto|first7=Y. K.|last8=Roccatagliata|first8=V.|last9=Sicilia-Aguilar|first9=A. |display-authors=6 |date=March 2012|title=Star formation and disk properties in Pismis 24|journal=Astronomy & Astrophysics|volume=539|page=A119|arxiv=1201.0833|bibcode=2012A&A...539A.119F|doi=10.1051/0004-6361/201015914|issn=0004-6361|s2cid=73612793}}</ref><ref name=Reed/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 404]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|78
|164,000
|14.14
|44,700
|분광법
|{{SIMBAD link|VFTS+404|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[웨스터하우트 51]]-2 ([[웨스터하우트 51]]에 존재)
|77
|20,000
|13.68<br/>{{small|(J&nbsp;대역)}}
|42,700
|항성진화 모델
|{{SIMBAD link|2MASS+J19230169%2B1416403|SIMBAD}}
|<ref name=Bik/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-68]] ([[대마젤란 은하]]의 [[BSDL 2505]]에 존재)
|76
|165,000
|14.13
|45,000
|분광법
|{{SIMBAD link|BAT99+68|SIMBAD}}
|<ref name="hainich" /><ref name=Bonanos/><ref group="lower-alpha">BSDL 2505는 대마젤란 은하의 성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[콜린더 228|HD 93632]] ([[용골자리 성운]]의 [[콜린더 228]]에 존재)
|76
|10,000
|8.23
|45,400
|항성진화 모델
|{{SIMBAD link|HD+93632|SIMBAD}}
|<ref name=Massey2001/><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[NGC 346]]-W3 ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|76
|200,000
|12.8
|52,500
|항성진화 모델
|{{SIMBAD link|Cl*+NGC+346+W+3|SIMBAD}}
|<ref name=Massey2000/><ref name="spitzer" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 169]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|76
|164,000
|14.437
|47,300
|분광법
|{{SIMBAD link|VFTS+169|SIMBAD}}
|<ref name="best" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 440]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|76
|164,000
|12.046
|39,800
|분광법
|{{SIMBAD link|VFTS+440|SIMBAD}}
|<ref name="best" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[AB1 (항성)|AB1]] ([[소마젤란 은하]]의 [[DEM S10]]에 존재)
|75
|197,000
|15.238
|79,000
|분광법
|{{SIMBAD link|SMC+AB+1|SIMBAD}}
|<ref name=Hainich2015>{{저널 인용|last1=Hainich|first1=R.|last2=Pasemann|first2=D.|last3=Todt|first3=H.|last4=Shenar|first4=T.|last5=Sander|first5=A.|last6=Hamann|first6=W. -R|date=2015|title=Wolf-Rayet stars in the Small Magellanic Cloud. I. Analysis of the single WN stars|journal=Astronomy & Astrophysics|volume=581|issue=21|page=30|arxiv=1507.04000|bibcode=2015A&A...581A..21H|doi=10.1051/0004-6361/201526241|s2cid=56230998}}</ref><ref name="spitzer" /><ref group="lower-alpha">DEM S10은 소마젤란 은하의 H II 영역이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 22]] A ([[용골자리 성운]]의 [[보훔 10]]에 존재)
|75
|8,300
| style="background:lightblue;color:darkblue;" |'''6.42'''<br/>{{small|(연성계 전체)}}
|44,700
|항성진화 모델
|{{SIMBAD link|WR+22|SIMBAD}}
|<ref name="hamann2019" /><ref name="ducati" /><ref group="lower-alpha" name="WR22">보훔 10은 용골자리 성운의 산개성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[피스미스 24-1]]NE ([[NGC 6357]]의 [[피스미스 24]]에 존재)
|74
|6,500
|11
|42,500
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|CL+PISMIS+24-1NE|SIMBAD}}
|<ref name="fang" /><ref name="skiff">{{저널 인용|last1=Skiff|first1=B. A.|date=October 2014|title=VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009- )|journal=VizieR On-Line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014)|volume=1|bibcode=2014yCat....1.2023S|s2cid=215961366}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 608]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|74
|164,000
|14.22
|42,200
|분광법
|{{SIMBAD link|VFTS+608|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-31]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|73
|163,000
|14.12
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+31|SIMBAD}}
|<ref name=Brands2022/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[머서 30]]-3 ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재)
|73
|40,000
|12.62<br/>{{small|(J&nbsp;대역)}}
|39,300
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-3|SIMBAD}}
|<ref name=Fuente/><ref group=lower-alpha name=Mc30/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[머서 30]]-11 ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재)
|73
|40,000
|12.33<br/>{{small|(J&nbsp;대역)}}
|36,800
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-11|SIMBAD}}
|<ref name=Fuente/><ref group=lower-alpha name=Mc30/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 566]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|73
|164,000
|14.05
|44,700
|분광법
|{{SIMBAD link|VFTS+566|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 64]]-16 ([[대마젤란 은하]]의 [[NGC 2001]]에 존재)
|72
|160,000
|13.666
|50,900
|항성진화 모델
|{{SIMBAD link|L72+LH+64-16|SIMBAD}}
|<ref name=Massey2000/><ref name="Zaritsky" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[NGC 2044]]-W35 ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|72
|160,000
|14.1
|48,200
|항성진화 모델
|{{SIMBAD link|WDP99+NGC+2044W+35|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 216]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|72
|164,000
|14.389
|44,700
|분광법
|{{SIMBAD link|VFTS+216|SIMBAD}}
|<ref name="best" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST2-1]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|71
|160,000
|14.3
|44,100
|항성진화 모델
|{{SIMBAD link|ST92+2-1|SIMBAD}}
|<ref name=Massey2000/><ref name="Schild" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[VFTS 3]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|71
|164,000
|11.56
|21,000
|분광법
|{{SIMBAD link|VFTS+3|SIMBAD}}
|<ref name=McEvoy>{{저널 인용|last1=McEvoy |first1=C.M. |last2=Dufton |first2=P.L. |last3=Evans |first3=C.J. |last4=Kalari |first4=V.M. |last5=Markova |first5=N.|last6=Simón-Díaz |first6=S. |last7=Vink|first7=J.S. |last8=Walborn |first8=N.R. |last9=Crowther |first9=P.A. |last10=de Koter |first10=A. |last11=de Mink |first11=S.E. |last12=Dunstall |first12=P.R. |last13=Hénault-Brunet |first13=V. |last14=Herrero |first14=A. |last15=Langer |first15=N. |last16=Lennon |first16=D. J.|last17=Maíz Apellániz |first17=J. |last18=Najarro |first18=F. |last19=Puls |first19=J. |last20=Sana|first20=H. |last21=Schneider |first21=F.R.N. |last22=Taylor|first22=W.D. |display-authors=6 |date=March 2015|title=The VLT-FLAMES Tarantula Survey: XIX. B-type supergiants: Atmospheric parameters and nitrogen abundances to investigate the role of binarity and the width of the main sequence⋆|journal=Astronomy & Astrophysics|volume=575|page=A70|doi=10.1051/0004-6361/201425202|issn=0004-6361|arxiv=1412.2705|bibcode=2015A&A...575A..70M|s2cid=39125418}}</ref><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[아치스 성단|아치스]]-F12 ([[아치스 성단]]에 존재하는 WR 102af)
|70
|25,000
|16.4<br/>{{small|(J&nbsp;대역)}}
|36,900
|분광법
|{{SIMBAD link|FNG2002+12|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 15629]] ([[하트 성운]]의 [[IC 1805]]에 존재)
|70
|7,500
|8.42
|45,900
|분광법
|{{SIMBAD link|HD+15629|SIMBAD}}
|<ref name=debecker/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 37974]] ([[대마젤란 은하]]의 [[N135]]에 존재)
|70
|163,000
|10.99
|22,500
|분광법
|{{SIMBAD link|HD+37974|SIMBAD}}
|<ref name="kastner">{{저널 인용|last1=Kastner|first1=Joel H.|last2=Buchanan|first2=Catherine L.|last3=Sargent|first3=B.|last4=Forrest|first4=W. J.|date=10 February 2006|title=Spitzer Spectroscopy of Dusty Disks around B[e] Hypergiants in the Large Magellanic Cloud|journal=The Astrophysical Journal|language=en|volume=638|issue=1|pages=L29–L32|bibcode=2006ApJ...638L..29K|doi=10.1086/500804|issn=0004-637X|s2cid=121769413|doi-access=free}}</ref><ref name="zacharias" /><ref group="lower-alpha">N135는 대마젤란 은하의 방출성운이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 93129]] Ab ([[용골자리 성운]]의 [[트럼플러 14]]에 존재)
|70
|7,500
|7.31<br/>{{small|(연성계 전체)}}
|44,000
|케플러의 법칙<br>(삼중성)
|{{SIMBAD link|HD+93129A|SIMBAD}}
|<ref name="nelan" /><ref name=tycho2>{{저널 인용|last1=Høg |first1=E. |last2=Fabricius |first2=C. |last3=Makarov |first3=V.V. |last4=Urban |first4=S. |last5=Corbin |first5=T. |last6=Wycoff |first6=G. |last7=Bastian |first7=U. |last8=Schwekendiek |first8=P. |last9=Wicenec |first9=A. |display-authors=6 |date=March 2000 |title=The Tycho-2 catalogue of the 2.5&nbsp;million brightest stars |journal=Astronomy & Astrophysics |volume=355 |pages=L27–L30 |bibcode=2000A&A...355L..27H |issn=0004-6361 |s2cid=17128864}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[M33 X-7]] B ([[삼각형자리 은하]]에 존재)
|70
|2,700,000
|18.7
|35,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|M33+X-7|SIMBAD}}
|<ref>{{저널 인용|last1=Orosz|first1=Jerome A.|last2=McClintock|first2=Jeffrey E.|last3=Narayan|first3=Ramesh|last4=Bailyn|first4=Charles D.|last5=Hartman|first5=Joel D.|last6=Macri|first6=Lucas|last7=Liu|first7=Jiefeng|last8=Pietsch|first8=Wolfgang|last9=Remillard|first9=Ronald A.|last10=Shporer|first10=Avi|last11=Mazeh|first11=Tsevi |display-authors=6 |date=October 2007|title=A 15.65-solar-mass black hole in an eclipsing binary in the nearby spiral galaxy M 33|journal=Nature|language=en|volume=449|issue=7164|pages=872–875|arxiv=0710.3165|bibcode=2007Natur.449..872O|doi=10.1038/nature06218|issn=0028-0836|pmid=17943124|s2cid=4311574}}</ref><ref>{{저널 인용|last1=Grimm|first1=H.-J.|last2=McDowell|first2=J.|last3=Zezas|first3=A.|last4=Kim|first4=D.-W.|last5=Fabbiano|first5=G.|date=December 2005|title=The X-Ray Binary Population in M33. I. Source List and Luminosity Function|journal=The Astrophysical Journal Supplement Series|language=en|volume=161|issue=2|pages=271–303|arxiv=astro-ph/0506353|bibcode=2005ApJS..161..271G|doi=10.1086/468185|issn=0067-0049|s2cid=119381693}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[Sk -69° 194]] A ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|70
|160,000
|12.131<br/>{{small|(연성계 전체)}}
|45,000
|항성진화 모델
|{{SIMBAD link|Sk+-69+194|SIMBAD}}
|<ref name=Massey2000/><ref name="Ulaczyk">{{저널 인용|last1=Ulaczyk |first1=K. |last2=Szymański |first2=M.K. |last3=Udalski |first3=A. |last4=Kubiak |first4=M. |last5=Pietrzyński |first5=G. |last6=Soszyński |first6=I. |last7=Wyrzykowski |first7=Ł. |last8=Poleski |first8=R. |last9=Gieren |first9=W. |last10=Walker |first10=A.R. |last11=Garcia-Varela |first11=A. |display-authors=6 |date=1 June 2013|title=Variable Stars from the OGLE-III Shallow Survey in the Large Magellanic Cloud|journal=Acta Astronomica|volume=63|issue=2|pages=159–179|arxiv=1306.4802|bibcode=2013AcA....63..159U|issn=0001-5237|s2cid=119228254}}</ref><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 125]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|69.6
|164,000
|16.6
|55,200
|분광법
|{{SIMBAD link|VFTS+125|SIMBAD}}
|<ref name="schneider2018" /><ref name="Schild" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 46150]] ([[장미 성운]]의 [[NGC 2244]]에 존재)
|69
|5,200
|6.73
|44,000
|분광법
|{{SIMBAD link|HD+46150|SIMBAD}}
|<ref name="fulltext" /><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[버클리 87|HD 229059]] ([[버클리 87]]에 존재)
|69
|3,000
|8.7
|26,300
|항성진화 모델
|{{SIMBAD link|HD+229059|SIMBAD}}
|<ref name=Massey2001/><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST2-3]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|69
|160,000
|14.264
|44,900
|항성진화 모델
|{{SIMBAD link|ST92+2-3|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST2-32]] ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|69
|160,000
|13.903
|45,400
|항성진화 모델
|{{SIMBAD link|ST92+2-32|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[W28-23]] ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|69
|160,000
|13.702
|51,300
|항성진화 모델
|{{SIMBAD link|W61+28-23|SIMBAD}}
|<ref name=Massey2000/><ref name="Zaritsky" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 93403]] A ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|68.5
|10,400
|8.27<br/>{{small|(연성계 전체)}}
|39,300
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|HD+93403|SIMBAD}}
|<ref name="rauw2000">{{저널 인용|last1=Rauw |first1=G. |last2=Sana |first2=H. |last3=Gosset |first3=E. |last4=Vreux |first4=J.-M. |last5=Jehin |first5=E. |last6=Parmentier |first6=G. |date=August 2000|title=A new orbital solution for the massive binary system HD&nbsp;93403 |journal=Astronomy & Astrophysics|volume=360 |pages=1003–1010 |bibcode=2000A&A...360.1003R |issn=0004-6361 |s2cid=13886945}}</ref><ref name="zacharias" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[콜린더 228|HD 93130]] ([[용골자리 성운]]의 [[콜린더 228]]에 존재)
|68
|10,000
|8.04
|39,900
|항성진화 모델
|{{SIMBAD link|HD+93130|SIMBAD}}
|<ref name=Massey2001/><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HM 1]]-8 ([[HM 1]]에 존재)
|68
|11,000
|12.52
|46,100
|항성진화 모델
|{{SIMBAD link|Cl+HM+1+8|SIMBAD}}
|<ref name=Massey2001/><ref name=Reed/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-47]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|68
|163,000
|14.72
|43,500
|항성진화 모델
|{{SIMBAD link|HSH95+47|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-48]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|68
|163,000
|14.75
|46,500
|항성진화 모델
|{{SIMBAD link|HSH95+48|SIMBAD}}
|<ref name=Brands2022/><ref name=crowther2016/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[웨스터하우트 51]]-61 ([[웨스터하우트 51]]에 존재)
|68
|20,000
|18.16<br/>{{small|(J&nbsp;대역)}}
|38,000
|항성진화 모델
|{{SIMBAD link|SSTOERC+G049.4836-00.4060|SIMBAD}}
|<ref name=Bik/><ref name=2MASS/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-93]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|67
|165,000
|13.446
|45,000
|분광법
|{{SIMBAD link|BAT99+93|SIMBAD}}
|<ref name="hainich" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[Sk -69° 200]] ([[대마젤란 은하]]의 [[NGC 2033]]에 존재)
|67
|160,000
|11.18
|26,300
|항성진화 모델
|{{SIMBAD link|Sk+-69+200|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[아치스 성단|아치스]]-F18 ([[아치스 성단]]에 존재)
|66.9
|25,000
|16.7<br/>{{small|(J&nbsp;대역)}}
|36,900
|분광법
|{{SIMBAD link|FNG2002+18|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[아치스 성단|아치스]]-F4 ([[아치스 성단]]에 존재하는 WR 102al)
|66.4
|25,000
|15.63<br/>{{small|(J&nbsp;대역)}}
|36,800
|분광법
|{{SIMBAD link|FNG2002+4|SIMBAD}}
|<ref name=grafener/><ref name=Figer/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-59]] A ([[대마젤란 은하]]의 [[NGC 2020]]에 존재)
|66
|165,000
|13.186<br/>{{small|(연성계 전체)}}
|71,000
|분광법
|{{SIMBAD link|BAT99+59|SIMBAD}}
|<ref name=hainich/><ref name=Bonanos/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-104]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|66
|165,000
|12.5
|63,000
|분광법
|{{SIMBAD link|BAT99+104|SIMBAD}}
|<ref name=hainich/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[HD 5980]] B ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|66
|200,000
|11.31<br/>{{small|(연성계 전체)}}
|45,000
|케플러의 법칙<br>(삼중성)
|{{SIMBAD link|HD+5980|SIMBAD}}
|<ref name="shenar">{{저널 인용|last1=Shenar |first1=T. |last2=Hainich |first2=R. |last3=Todt |first3=H. |last4=Sander |first4=A. |last5=Hamann |first5=W.-R. |last6=Moffat |first6=A.F.J. |last7=Eldridge |first7=J.J. |last8=Pablo |first8=H.|last9=Oskinova |first9=L.M. |last10=Richardson |first10=N.D. |display-authors=6 |date=July 2016|title=Wolf-Rayet stars in the Small Magellanic Cloud: II. Analysis of the binaries |journal=Astronomy & Astrophysics |volume=591 |page=A22 |arxiv=1604.01022 |bibcode=2016A&A...591A..22S |doi=10.1051/0004-6361/201527916 |issn=0004-6361 |s2cid=119255408}}</ref><ref name="tycho2" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 190429]] A ([[바너드 146]] 근처에 존재)
|66
|7,800
|6.63<br/>{{small|(연성계 전체)}}
|46,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|HD+190429A|SIMBAD}}
|<ref name="bouret2">{{저널 인용|last1=Bouret |first1=J.-C. |last2=Hillier |first2=D.J. |last3=Lanz |first3=T. |last4=Fullerton |first4=A.W. |year=2012 |title=Properties of galactic early-type O-supergiants: A combined FUV-UV and optical analysis |journal=[[Astronomy & Astrophysics]] |volume=544 |page=A67 |arxiv=1205.3075 |bibcode=2012A&A...544A..67B |doi=10.1051/0004-6361/201118594 |s2cid=119280104}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 31]]-1003 ([[대마젤란 은하]]의 [[NGC 1858]]에 존재)
|66
|160,000
|13.186
|41,900
|항성진화 모델
|{{SIMBAD link|L72+LH+31-1003|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 114]]-7 ([[대마젤란 은하]]의 [[N70 (성운)|N70]]에 존재)
|66
|160,000
|13.66
|50,000
|분광법
|{{SIMBAD link|L72+LH+114-7|SIMBAD}}
|<ref name=fulltext/><ref name=Bonanos/><ref group="lower-alpha">N70은 대마젤란 은하의 방출성운이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[피스미스 24-1]]SW ([[NGC 6357]]의 [[피스미스 24]]에 존재)
|66
|6,500
|11.1
|40,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|CL+PISMIS+24-1SW|SIMBAD}}
|<ref name=fang/><ref name=skiff/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-126]] ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|65
|165,000
|13.166
|71,000
|분광법
|{{SIMBAD link|BAT99+126|SIMBAD}}
|<ref name=hainich/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-40]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|163,000
|14.56
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+40|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-58]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|163,000
|14.8
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+58|SIMBAD}}
|<ref name="Brands2022" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-89]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|163,000
|14.76
|44,000
|분광법
|{{SIMBAD link|HSH95+89|SIMBAD}}
|<ref name="crowther2016" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 63]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|164,000
|14.4
|42,200
|분광법
|{{SIMBAD link|VFTS+63|SIMBAD}}
|<ref name="best" /><ref name="Schild" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 145]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|164,000
|14.3
|39,800
|분광법
|{{SIMBAD link|VFTS+145|SIMBAD}}
|<ref name="best" /><ref name="Doran2013" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 518]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|65
|164,000
|15.11
|44,700
|분광법
|{{SIMBAD link|VFTS+518|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[웨스터하우트 49]]-8 ([[웨스터하우트 49]]에 존재)
|65
|36,200
|15.617<br/>{{small|(J&nbsp;대역)}}
|40,700
|항성진화 모델
|{{SIMBAD link|WBB2016+8|SIMBAD}}
|<ref name=Wu2016/><ref name=2MASS/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[BD+43° 3654]] ([[백조자리 OB2]]에 존재하는 [[폭주성]])
|64.6
|5,400
|10.06
|40,400
|항성진화 모델
|{{SIMBAD link|BD%2B43+3654|SIMBAD}}
|<ref name="comeron">{{저널 인용|last1=Comerón|first1=F.|last2=Pasquali|first2=A.|date=July 2012|title=New members of the massive stellar population in Cygnus|journal=Astronomy & Astrophysics|volume=543|page=A101|bibcode=2012A&A...543A.101C|doi=10.1051/0004-6361/201219022|issn=0004-6361|s2cid=73520813|doi-access=free}}</ref><ref name="tycho2" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-129]] A ([[대마젤란 은하]]의 [[DEM L294]]에 존재)
|64
|165,000
|14.701<br/>{{small|(연성계 전체)}}
|79,000
|분광법
|{{SIMBAD link|BAT99+129|SIMBAD}}
|<ref name="hainich" /><ref name=Bonanos/><ref group="lower-alpha">DEM L294는 대마젤란 은하의 H II 영역이다.</ref><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-50]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|64
|163,000
|14.65
|47,000
|항성진화 모델
|{{SIMBAD link|HSH95+50|SIMBAD}}
|<ref name=Brands2022/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -69° 25]] ([[대마젤란 은하]]의 [[NGC 1748]]에 존재)
|64
|160,000
|11.886
|43,600
|항성진화 모델
|{{SIMBAD link|Sk+-69+25|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[트럼플러 27]]-23 ([[트럼플러 27]]에 존재)
|64
|3,900
|10.09
|27,500
|항성진화 모델
|{{SIMBAD link|Cl+Trumpler+27+23|SIMBAD}}
|<ref name=Massey2001/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[웨스터하우트 49]]-5 ([[웨스터하우트 49]]에 존재)
|64
|36,200
|15.623<br/>{{small|(J&nbsp;대역)}}
|42,700
|항성진화 모델
|{{SIMBAD link|WBB2016+5|SIMBAD}}
|<ref name=Wu2016/><ref name=2MASS/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 46223]] ([[장미 성운]]의 [[NGC 2244]]에 존재)
|63
|5,200
|7.28
|46,000
|분광법
|{{SIMBAD link|HD+46223|SIMBAD}}
|<ref name="fulltext" /><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HD 64568]] ([[고물자리 OB2]]의 [[NGC 2467]]에 존재)
|63
|16,000
|9.39
|54,000
|분광법
|{{SIMBAD link|HD+64568|SIMBAD}}
|<ref name="fulltext" /><ref name="zacharias" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[트럼플러 16|HD 303308]] ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
|63
|9,200
|8.17
|51,300
|항성진화 모델
|{{SIMBAD link|HD+303308|SIMBAD}}
|<ref name=Massey2001/><ref name="zacharias" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HR 6187]] A ([[제단자리 OB1]]의 [[NGC 6193]]에 존재)
|63
|4,300
| style="background:lightblue;color:darkblue;" |'''5.54'''<br/>{{small|(연성계 전체)}}
|46,500
|Septenary
|{{SIMBAD link|HR+6187|SIMBAD}}
|<ref name="krticka">{{저널 인용|last1=Krtička |first1=J. |last2=Kubát |first2=J. |last3=Krtičková |first3=I. |date=July 2015 |title=X-ray irradiation of the winds in binaries with massive components |journal=Astronomy & Astrophysics |volume=579 |page=A111 |arxiv=1505.03411 |bibcode=2015A&A...579A.111K |doi=10.1051/0004-6361/201525637 |issn=0004-6361 |s2cid=119120927}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 10]]-3058 ([[대마젤란 은하]]의 [[NGC 1763]]에 존재)
|63
|160,000
|14.089
|54,000
|분광법
|{{SIMBAD link|PGMW+3058|SIMBAD}}
|<ref name="fulltext" /><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST5-71]] ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
|63
|160,000
|13.266
|45,400
|항성진화 모델
|{{SIMBAD link|ST92+5-71|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[AB9 (항성)|AB9]] ([[소마젤란 은하]]의 [[DEM S80]]에 존재)
|62
|197,000
|15.431
|100,000
|분광법
|{{SIMBAD link|SMC+AB+9|SIMBAD}}
|<ref name=Hainich2015/><ref name="spitzer" /><ref group="lower-alpha">DEM S80은 소마젤란 은하의 H II 영역이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[브레이 32]] B ([[대마젤란 은하]]의 [[NGC 1966]]에 존재)
|62
|165,000
|12.32<br/>{{small|(연성계 전체)}}
|43,600
|항성진화 모델
|{{SIMBAD link|Brey+32|SIMBAD}}
|<ref name=Massey2000/><ref name="zacharias" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[트럼플러 14|HD 93160]] ([[용골자리 성운]]의 [[트럼플러 14]]에 존재)
|62
|8,000
|7.6
|42,700
|항성진화 모델
|{{SIMBAD link|HD+93160|SIMBAD}}
|<ref name=Massey2001/><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-35]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|62
|163,000
|14.43
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+35|SIMBAD}}
|<ref name=Brands2022/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 41]]-1017 ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|62
|160,000
|12.266
|42,700
|항성진화 모델
|{{SIMBAD link|L72+LH+41-1017|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[머서 30]]-6a A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-4 A)
|62
|40,000
|10.39<br/>{{small|(J&nbsp;대역)}}
|29,900
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-6a|SIMBAD}}
|<ref name=Fuente/><ref group=lower-alpha name=Mc30/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST4-18]] ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|62
|160,000
|13.639
|44,800
|항성진화 모델
|{{SIMBAD link|ST92+4-18|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 664]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|62
|164,000
|13.937
|39,900
|분광법
|{{SIMBAD link|VFTS+664|SIMBAD}}
|<ref name=best/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[백조자리 OB9|HD 229196]] ([[백조자리 OB9]]에 존재)
|61.6
|5,000
|8.59
|40,900
|항성진화 모델
|{{SIMBAD link|HD+229196|SIMBAD}}
|<ref name=comeron/><ref name=Reed/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[AB8 (항성)|AB8]] B ([[소마젤란 은하]]의 [[NGC 602]]에 존재)
|61
|197,000
|12.83<br/>{{small|(연성계 전체)}}
|45,000
|케플러의 법칙<br>(쌍성)
|{{SIMBAD link|SMC+AB+8|SIMBAD}}
|<ref name="shenar" /><ref>{{저널 인용|last=Massey|first=Philip|date=July 2002|title=A UBVR CCD Survey of the Magellanic Clouds|journal=The Astrophysical Journal Supplement Series|language=en|volume=141|issue=1|pages=81–122|arxiv=astro-ph/0110531|bibcode=2002ApJS..141...81M|doi=10.1086/338286|issn=0067-0049|s2cid=119447348}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[BAT99-79]] A ([[대마젤란 은하]]의 [[NGC 2044]]에 존재)
|61
|165,000
|13.486<br/>{{small|(연성계 전체)}}
|42,000
|분광법
|{{SIMBAD link|BAT99+79|SIMBAD}}
|<ref name="hainich" /><ref name=Bonanos/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[HD 5980]] A ([[소마젤란 은하]]의 [[NGC 346]]에 존재)
|61
|200,000
|11.31<br/>{{small|(연성계 전체)}}
|21,000–53,000
|케플러의 법칙<br>(삼중성)
|{{SIMBAD link|HD+5980|SIMBAD}}
|<ref name=shenar/><ref name=tycho2/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[LH 41]]-18 ([[대마젤란 은하]]의 [[NGC 1910]]에 존재)
|61
|160,000
|12.586
|38,500
|항성진화 모델
|{{SIMBAD link|L72+LH+41-18|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[머서 30]]-9 A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재)
|61
|40,000
|12.25<br/>{{small|(J&nbsp;대역)}}
|34,500
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-9|SIMBAD}}
|<ref name=Fuente/><ref group=lower-alpha name=Mc30/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[ST5-25]] ([[대마젤란 은하]]의 [[NGC 2074]]에 존재)
|61
|160,000
|13.551
|48,600
|항성진화 모델
|{{SIMBAD link|ST92+5-25|SIMBAD}}
|<ref name=Massey2000/><ref name=Zaritsky/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[VFTS 422]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|61
|164,000
|15.14
|39,800
|분광법
|{{SIMBAD link|VFTS+422|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[다섯쌍둥이 성단|WR 102hb]] ([[다섯쌍둥이 성단]]에 존재)
|61
|26,000
|13.9<br/>{{small|(J&nbsp;대역)}}
|25,100
|항성진화 모델
|{{SIMBAD link|WR+102hb|SIMBAD}}
|<ref name=Liermann>{{저널 인용|last1=Liermann |first1=Adriane|last2=Hamann |first2=Wolf-Rainer |last3=Oskinova |first3=Lidia M. |last4=Todt |first4=Helge |date=January 2011 |title=High-mass stars in the Galactic center Quintuplet cluster |journal=Société Royale des Sciences de Liège, Bulletin |volume=80 |pages=160–164 |bibcode=2011BSRSL..80..160L |issn=0037-9565 |s2cid=116895316}}</ref><ref name="qc">{{저널 인용|last1=Clark |first1=J.S. |last2=Lohr |first2=M.E. |last3=Patrick |first3=L.R. |last4=Najarro |first4=F. |last5=Dong |first5=H. |last6=Figer |first6=D.F. |date=October 2018 |title=An updated stellar census of the Quintuplet cluster |journal=Astronomy & Astrophysics |volume=618 |page=A2 |arxiv=1805.10139 |bibcode=2018A&A...618A...2C |doi=10.1051/0004-6361/201833041 |issn=0004-6361 |s2cid=53501337}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -67° 166]] ([[대마젤란 은하]]의 [[GKK-A144]]에 존재)
|60.68
|160,000
|12.22
|41,800
|분광법
|{{SIMBAD link|Sk+-67+166|SIMBAD}}
|<ref name=Massa2017/><ref name=Bonanos/><ref group="lower-alpha" name="A144">GKK-A144는 대마젤란 은하의 성협이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -67° 167]] ([[대마젤란 은하]]의 [[GKK-A144]]에 존재)
|60.68
|160,000
|12.586
|41,800
|분광법
|{{SIMBAD link|Sk+-67+167|SIMBAD}}
|<ref name=Massa2017/><ref name=Bonanos/><ref group=lower-alpha name=A144/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[Sk -71° 46]] ([[대마젤란 은하]]의 [[BSDL 2242]]에 존재)
|60.68
|160,000
|13.241
|41,800
|분광법
|{{SIMBAD link|Sk+-71+46|SIMBAD}}
|<ref name=Massa2017/><ref name=Bonanos/><ref group="lower-alpha">BSDL 2242는 대마젤란 은하의 성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[브레이 10]] ([[대마젤란 은하]]의 [[NGC 1770]]에 존재)
|60
|165,000
|12.69
|117,000
|항성진화 모델
|{{SIMBAD link|Brey+10|SIMBAD}}
|<ref name=Massey2000/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[브레이 94]] A ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|60
|165,000
|12.996<br/>{{small|(연성계 전체)}}
|83,000
|항성진화 모델
|{{SIMBAD link|Brey+94|SIMBAD}}
|<ref name=Massey2000/><ref name=Bonanos/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[브레이 95a]] A ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|60
|165,000
|12.2<br/>{{small|(연성계 전체)}}
|83,000
|항성진화 모델
|{{SIMBAD link|Brey+95a|SIMBAD}}
|<ref name=Massey2000/><ref name=Testor>{{저널 인용|last1=Testor |first1=G. |last2=Niemela |first2=V. |date=June 1998 |title=The OB associations LH 101 and LH 104 in the HII region N158 of the LMC |journal=Astronomy and Astrophysics Supplement Series |volume=130 |issue=3 |pages=527–538 |bibcode=1998A&AS..130..527T |doi=10.1051/aas:1998241 |issn=0365-0138 |s2cid=55801387 |doi-access=free}}</ref><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[HSH95-55]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|60
|163,000
|14.74
|47,500
|항성진화 모델
|{{SIMBAD link|HSH95+55|SIMBAD}}
|<ref name=Brands2022/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[머서 30]]-7 A ([[드래곤피쉬 성운]]의 [[머서 30]]에 존재하는 WR 46-5 A)
|60
|40,000
|11.516<br/>{{small|(J&nbsp;대역)}}
|41,400
|항성진화 모델
|{{SIMBAD link|DNB2016+Mc30-7|SIMBAD}}
|<ref name=Fuente/><ref group=lower-alpha name=Mc30/><ref name="Binary" group="lower-alpha" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[R134 (항성)|R134]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|60
|164,000
|12.75
|39,800
|분광법
|{{SIMBAD link|RMC134|SIMBAD}}
|<ref name=best/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[R142 (항성)|R142]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|60
|164,000
|11.82
|18,000
|분광법
|{{SIMBAD link|RMC142|SIMBAD}}
|<ref name=McEvoy/><ref name=Doran2013/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[R143 (항성)|R143]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|60
|160,000
|12.014
|18,000–36,000
|항성진화 모델
|{{SIMBAD link|RMC143|SIMBAD}}
|<ref name=Smith2015/><ref name=Bonanos/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[Sk -69° 142a]] ([[대마젤란 은하]]의 [[NGC 1983]]에 존재)
|60
|160,000
|11.093
|34,000
|항성진화 모델
|{{SIMBAD link|Sk+-69+142a|SIMBAD}}
|<ref name=Smith2015/><ref name=Ulaczyk/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[Sk -69° 259]] ([[대마젤란 은하]]의 [[NGC 2081]]에 존재)
|60
|160,000
|11.93
|23,000
|항성진화 모델
|{{SIMBAD link|Sk+-69+259|SIMBAD}}
|<ref name=Massey2000/><ref name=zacharias/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[Var 83]] ([[삼각형자리 은하]]에 존재)
|60
|3,000,000
|16.027
|18,000–37,000
|항성진화 모델
|{{SIMBAD link|VHK+83|SIMBAD}}
|<ref name=burggraf>{{콘퍼런스 인용|last1=Burggraf |first1=B. |last2=Weis |first2=K. |last3=Bomans |first3=D.J. |date=December 2006 |title=LBVs in M33: Their environments and ages |book-title=Stellar Evolution at Low Metallicity: Mass loss, explosions, cosmology |series=ASP Conference Series |volume=353 |page=245 |bibcode=2006ASPC..353..245B |issn=1050-3390 |s2cid=230292777 |publisher=[[Astronomical Society of the Pacific]]}}</ref><ref>{{저널 인용|last1=Massey |first1=Philip |last2=Neugent |first2=Kathryn F. |last3=Smart |first3=Brianna M. |date=19 August 2016 |title=A spectroscopic survey of massive stars in M31 and M33 |journal=[[The Astronomical Journal]] |volume=152 |issue=3 |page=62 |arxiv=1604.00112 |bibcode=2016AJ....152...62M |doi=10.3847/0004-6256/152/3/62 |issn=1538-3881 |s2cid=35672588 |doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[VFTS 430]] ([[대마젤란 은하]]의 [[타란툴라 성운]]에 존재)
|60
|164,000
|15.11
|24,500
|분광법
|{{SIMBAD link|VFTS+430|SIMBAD}}
|<ref name=McEvoy/><ref name=Doran2013/>
|}


비교 목적으로 질량이 60 {{태양질량|link=y}} 미만인 몇 가지 유명한 큰 별이 아래 표에 표시되어 있으며 매우 가깝지만 목록에 포함하기에는 너무 작은 [[태양]]으로 끝난다. 현재 나열된 모든 별은 육안으로 볼 수 있으며 비교적 가까이 있다.

{| class="wikitable sortable"
|-
! 항성 이름
! [[질량]]
({{태양질량|link=y}}, [[태양]] = 1)
! 대략 태양계로부터의 거리([[광년]])
! [[겉보기등급]]
! [[표면온도|유효온도]] ([[켈빈|K]])
! 분석 방식
! 링크
! 참고문헌
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[나오스]] ([[돛자리 분자 능선]]의 [[돛자리 R2]]에 존재)
|56.1
|1,080
| style="background:lightblue;color:darkblue;" |'''2.25'''
|40,000
|분광법
|{{SIMBAD link|Zeta+Puppis|SIMBAD}}
|<ref name="bouret2" /><ref name="ducati" /><ref group="lower-alpha">돛자리 R2는 돛자리 분자 능선의 OB 성협이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[세페우스자리 람다]] ([[세페우스자리 OB3]]에 존재하는 [[폭주성]])
|51.4
|3,100
| style="background:lightblue;color:darkblue;" |'''5.05'''
|36,000
|분광법
|{{SIMBAD link|Lambda+Cephei|SIMBAD}}
|<ref name="bouret2" /><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[큰개자리 타우]] Aa ([[NGC 2362]]에 존재)
|50
|5,120
| style="background:lightblue;color:darkblue;" |'''4.89'''
|32,000
|항성진화 모델
|{{SIMBAD link|Tau+Canis+Majoris|SIMBAD}}
|<ref name=devries>{{저널 인용|arxiv=1309.1475 |doi=10.1093/mnras/stt1688 |title=The evolution of triples with a Roche lobe filling outer star |journal=Monthly Notices of the Royal Astronomical Society |volume=438 |issue=3 |page=1909 |year=2014 |last1=de Vries |first1=N. |last2=Portegies Zwart |first2=S. |last3=Figueira |first3=J. |bibcode=2014MNRAS.438.1909D}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[파리자리 세타]] Ab ([[센타우루스자리 OB1]]에 존재)
|44
|7,400
| style="background:lightblue;color:darkblue;" |'''5.53'''<br/>{{small|(연성계 전체)}}
|33,000
|항성진화 모델
|{{SIMBAD link|Theta+Muscae+A|SIMBAD}}
|<ref>{{저널 인용|last1=Hill|first1=G. M.|last2=Moffat|first2=A. F. J.|last3=St-Louis|first3=N.|date=1 October 2002|title=Modelling the colliding-winds spectra of the 19-d WR + OB binary in the massive triple system θ Muscae|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=335|issue=4|pages=1069–1078|bibcode=2002MNRAS.335.1069H|doi=10.1046/j.1365-8711.2002.05694.x|issn=0035-8711|s2cid=121923927|doi-access=free}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[알닐람]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|40
|2,000
| style="background:lightblue;color:darkblue;" |'''1.69'''
|27,500
|항성진화 모델
|{{SIMBAD link|Epsilon+Orionis|SIMBAD}}
|<ref>{{저널 인용 |last1=Zsargó |first1=J. |last2=Fierro-Santillán |first2=C.R. |last3=Klapp |first3=J. |last4=Arrieta |first4=A. |last5=Arias |first5=L. |last6=Valencia |first6=J.M. |last7=Sigalotti |first7=L. di G. |last8=Hareter |first8=M. |last9=Puebla |first9=R.E. |display-authors=6 |date=November 2020 |title=Creating and using large grids of precalculated model atmospheres for a rapid analysis of stellar spectra |journal=Astronomy & Astrophysics |volume=643 |page=A88 |arxiv=2009.10879 |bibcode=2020A&A...643A..88Z |doi=10.1051/0004-6361/202038066 |issn=0004-6361 |s2cid=225194447}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[오리온자리 세타2]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|39
|1,500
| style="background:lightblue;color:darkblue;" |'''5.02'''
|34,900
|항성진화 모델
|{{SIMBAD link|Theta2+Orionis+A|SIMBAD}}
|<ref name=mitschang>{{저널 인용 |last1=Mitschang |first1=Arik W. |last2=Schulz |first2=Norbert S.|last3=Huenemoerder|first3=David P.|last4=Nichols |first4=Joy S. |last5=Testa |first5=Paola |year=2011 |title=Detailed X-ray line properties of {{nobr|θ<sup>2</sup> Ori A}} in quiescence |journal=The Astrophysical Journal|volume=734 |issue=1 |page=14 |doi=10.1088/0004-637X/734/1/14 |s2cid=15568141 |bibcode=2011ApJ...734...14M |arxiv=1009.1896}}</ref><ref>{{저널 인용 |last1=Aldoretta |first1=E.J. |last2=Caballero-Nieves |first2=S.M. |last3=Gies |first3=D.R. |last4=Nelan |first4=E.P. |last5=Wallace |first5=D.J. |last6=Hartkopf |first6=W.I. |last7=Henry |first7=T.J. |last8=Jao |first8=W.-C. |last9=Maíz Apellániz |first9=J. |last10=Mason |first10=B.D. |last11=Moffat |first11=A.F.J. |last12=Norris |first12=R.P. |last13=Richardson |first13=N.D. |last14=Williams |first14=S.J. |display-authors=6 |year=2015 |title=The multiplicity of massive stars: A high angular-resolution survey with the guidance sensor |journal=The Astronomical Journal |volume=149 |issue=1 |page=26 |doi=10.1088/0004-6256/149/1/26 |arxiv=1410.0021 |s2cid=58911264 |bibcode=2015AJ....149...26A }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[기린자리 알파]] ([[NGC 1502]]에 존재하는 [[폭주성]])
|37.6
|6,000
| style="background:lightblue;color:darkblue;" |'''4.29'''
|29,000
|항성진화 모델
|{{SIMBAD link|Alpha+Camelopardalis|SIMBAD}}
|<ref name=repolust>{{저널 인용 |last1=Repolust |first1=T. |last2=Puls |first2=J. |last3=Herrero |first3=A. |date=February 2004 |title=Stellar and wind parameters of Galactic O-stars: The influence of line-blocking/blanketing |journal=Astronomy & Astrophysics |volume=415 |issue=1 |pages=349–376 |bibcode=2004A&A...415..349R |doi=10.1051/0004-6361:20034594 |issn=0004-6361 |s2cid=56418916 |doi-access=free}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WN}};text-align:left;" | [[백조자리 P]] ([[백조자리 OB1]]의 [[IC 4996]]에 존재)
|37
|5,100
| style="background:lightblue;color:darkblue;" |'''4.82'''
|18,700
|분광법
|{{SIMBAD link|P+Cygni|SIMBAD}}
|<ref name=rivet>{{저널 인용|bibcode=2020MNRAS.494..218R|arxiv=1910.08366|doi=10.1093/mnras/staa588|title=Intensity interferometry of P Cygni in the H α emission line: Towards distance calibration of LBV supergiant stars |year=2020 |last1=Rivet |first1=J-P |last2=Siciak |first2=A. |last3=de Almeida |first3=E.S.G. |last4=Vakili|first4=F. |last5=Domiciano de Souza |first5=A. |last6=Fouché |first6=M. |last7=Lai |first7=O. |last8=Vernet |first8=D. |last9=Kaiser |first9=R. |last10=Guerin |first10=W. |display-authors=6 |journal=Monthly Notices of the Royal Astronomical Society |volume=494 |issue=1 |pages=218–227 |s2cid=204788654}}</ref><ref name="ducati" /><ref group="lower-alpha">[[IC 4996]]은 백조자리 OB1의 산개성단이다.</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[전갈자리 제타1]] ([[전갈자리 OB1]]의 [[NGC 6231]]에 존재)
|36
|8,210
| style="background:lightblue;color:darkblue;" |'''4.705'''
|17,200
|분광법
|{{SIMBAD link|Zeta1+Scorpii|SIMBAD}}
|<ref name="clark"/><ref name="aass61_387">{{저널 인용 | last1=Kozok | first1=J. R. | title=Photometric observations of emission B-stars in the southern Milky Way | journal=Astronomy and Astrophysics Supplement Series | volume=61 | pages=387–405 |date=September 1985 | bibcode=1985A&AS...61..387K }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[알니탁]] Aa ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|33
|1,260
| style="background:lightblue;color:darkblue;" |'''2.08'''
|29,500
|항성진화 모델
|{{SIMBAD link|Zeta+Orionis|SIMBAD}}
|<ref>{{저널 인용|last1=Hummel|first1=C. A.|last2=Rivinius|first2=Th.|last3=Nieva|first3=M.-F.|last4=Stahl|first4=O.|last5=van Belle|first5=G.|last6=Zavala|first6=R. T.|date=2013|title=Dynamical mass of the O-type supergiant in ζ Orionis A|journal=Astronomy & Astrophysics|volume=554|page=A52|arxiv=1306.0330|bibcode=2013A&A...554A..52H|doi=10.1051/0004-6361/201321434|s2cid=53645495|issn=0004-6361}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[오리온자리 세타1 C]]1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[사다리꼴성단]]에 존재)
|33
|1,340
| style="background:lightblue;color:darkblue;" |'''5.13'''<br/>{{small|(연성계 전체)}}
|39,000
|항성진화 모델
|{{SIMBAD link|Theta1+Orionis+C|SIMBAD}}
|<ref name=balega2014>{{저널 인용 |last1=Balega |first1=Yu. Yu. |last2=Chentsov |first2=E.L. |last3=Leushin |first3=V.V. |last4=Rzaev |first4=A.Kh. |last5=Weigelt |first5=G. |title=Young massive binary θ{{sup|1}} Ori C: Radial velocities of components |journal=Astrophysical Bulletin |volume=69|issue=1 |year=2014 |pages=46–57|issn=1990-3413|doi=10.1134/S1990341314010052|bibcode=2014AstBu..69...46B|s2cid=120838635}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[카시오페이아자리 카파]] ([[카시오페아자리 OB14]]에 존재)
|33
| 4,000
| style="background:lightblue;color:darkblue;" |'''4.16'''
|23,500
|항성진화 모델
|{{SIMBAD link|Kappa+Cassiopeiae|SIMBAD}}
|<ref name="Searle 20082">{{저널 인용|author=Searle, S. C.|author2=Prinja, R. K.|author3=Massa, D.|author4=Ryans, R.|date=2008|title=Quantitative studies of the optical and UV spectra of Galactic early B supergiants. I. Fundamental parameters|journal=Astronomy and Astrophysics|volume=481|issue=3|pages=777–797|arxiv=0801.4289|bibcode=2008A&A...481..777S|doi=10.1051/0004-6361:20077125|s2cid=1552752}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[작각자자리 뮤]] ([[NGC 6169]]에 존재)
|33
| 3,260
| style="background:lightblue;color:darkblue;" |'''4.91'''
|28,000
|분광법
|{{SIMBAD link|Mu+Normae|SIMBAD}}
|<ref name=tetzlaff>{{저널 인용|bibcode= 2011MNRAS.410..190T|title= A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun|journal= Monthly Notices of the Royal Astronomical Society|volume= 410|pages= 190–200|last1= Tetzlaff|first1= N.|last2= Neuhäuser|first2= R.|last3= Hohle|first3= M. M.|year= 2011|issue= 1|doi= 10.1111/j.1365-2966.2010.17434.x|arxiv = 1007.4883 |s2cid= 118629873}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[용골자리 에타]] B ([[용골자리 성운]]의 [[트럼플러 16]]에 존재)
| 30
|7,500
| style="background:lightblue;color:darkblue;" |'''4.3'''<br/>{{small|(연성계 전체)}}
| 37,200
|Binary
|{{SIMBAD link|Eta+Carinae|SIMBAD}}
|<ref name="KashiSoker">{{저널 인용 |last1=Kashi |first1=Amit |last2=Soker |first2=Noam |date=1 November 2010 |title=Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae |journal=The Astrophysical Journal |volume=723 |issue=1 |pages=602–611 |arxiv=0912.1439 |bibcode=2010ApJ...723..602K |doi=10.1088/0004-637X/723/1/602 |issn=0004-637X |s2cid=118399302}}</ref><ref name="2018-07-02_NAL" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[돛자리 감마|돛자리 감마2]] B ([[돛자리 OB2]]에 존재)
|28.5
| 1,230
| style="background:lightblue;color:darkblue;" |'''1.83'''<br/>{{small|(연성계 전체)}}
|35,000
|항성진화 모델
|{{SIMBAD link|Gamma2+Velorum|SIMBAD}}
|<ref name=GammaVelorum/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[메이사]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 람다 성단|콜린더 69]]에 존재)
|27.9
| 1,100
| style="background:lightblue;color:darkblue;" |'''3.54'''
|37,700
|분광법
|{{SIMBAD link|Lambda+Orionis+A|SIMBAD}}
|<ref name=tetzlaff/><ref name=hr>{{서적 인용|last1=Hoffleit|first1=Dorrit|title=The Bright star catalogue|last2=Jaschek|first2=Carlos|publisher=Yale University Observatory|year=1991|edition=5th Revised|location=New Haven, Conn.|bibcode=1991bsc..book.....H}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[멘키브]] ([[페르세우스자리 OB2]]의 [[캘리포니아 성운|NGC 1499]]에 존재)
| 26.1
| 1,200
| style="background:lightblue;color:darkblue;" |'''4.04'''
| 35,000
|항성진화 모델
|{{SIMBAD link|Xi+Persei|SIMBAD}}
|<ref name=repolust/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 79a]] ([[전갈자리 OB1 성협|전갈자리 OB1]]의 [[NGC 6231]]에 존재)
|24.4
| 5,600
| style="background:lightblue;color:darkblue;" |'''5.77'''
|35,000
|분광법
|{{SIMBAD link|WR+79a|SIMBAD}}
|<ref name=tetzlaff/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[민타카]] Aa1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|24
| 1,200
| style="background:lightblue;color:darkblue;" |'''2.5'''<br/>{{small|(연성계 전체)}}
|29,500
|항성진화 모델
|{{SIMBAD link|Delta+Orionis+A|SIMBAD}}
|<ref name="shenar2015">{{저널 인용 |last1=Shenar|first1=T. |last2=Oskinova|first2=L. |last3=Hamann |first3=W.-R. |last4=Corcoran |first4=M.F. |last5=Moffat|first5=A.F.J. |last6=Pablo |first6=H. |last7=Richardson|first7=N.D. |last8=Waldron |first8=W.L. |last9=Huenemoerder |first9=D.P. |last10=Maíz Apellániz |first10=J. |last11=Nichols |first11=J.S. |last13=Nazé |first13=Y. |last14=Hoffman |first14=J.L. |last15=Pollock |first15=A.M.T. |last16=Negueruela |first16=I. |first12=H. |last12=Todt |display-authors=6 |year=2015 |title=A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis |journal=Astrophysical Journal |volume=809 |issue=2 |page=135 |arxiv=1503.03476 |bibcode=2015ApJ...809..135S |doi=10.1088/0004-637X/809/2/135|hdl=10045/59172|s2cid=14909574}}</ref><ref name="tokovinin1997">{{저널 인용 |bibcode=1997A&AS..124...75T |title=MSC - a catalogue of physical multiple stars |journal=Astronomy and Astrophysics Supplement Series |volume=124 |pages=75–84 |last1=Tokovinin |first1=A A. |year=1997 |doi=10.1051/aas:1997181|doi-access=free}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[하트샤]] Aa1 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[NGC 1980]]에 존재)
|23.1
| 1,340
| style="background:lightblue;color:darkblue;" |'''2.77'''<br/>{{small|(연성계 전체)}}
|32,500
|항성진화 모델
|{{SIMBAD link|Iota+Orionis|SIMBAD}}
|<ref name="marchenko">{{저널 인용|bibcode=2000MNRAS.317..333M|title=Coordinated monitoring of the eccentric O-star binary Iota Orionis: Optical spectroscopy and photometry|journal=Monthly Notices of the Royal Astronomical Society |volume=317 |issue=2 |page=333 |last1=Marchenko |first1=Sergey V. |last2=Rauw |first2=Gregor |last3=Antokhina |first3=Eleonora A. |last4=Antokhin |first4=Igor I.|last5=Ballereau |first5=Dominique |last6=Chauville |first6=Jacques |last7=Corcoran |first7=Michael F.|last8=Costero |first8=Rafael |last9=Echevarria |first9=Juan |last10=Eversberg |first10=Thomas |last11=Gayley |first11=Ken G. |last12=Koenigsberger |first12=Gloria |author12-link=Gloria Suzanne Koenigsberger Horowitz|last13=Miroshnichenko|first13=Anatoly S. |last14=Moffat |first14=Anthony F.J. |last15=Morrell |first15=Nidia I. |last16=Morrison |first16=Nancy D. |last17=Mulliss |first17=Christopher L. |last18=Pittard |first18=Julian M. |last19=Stevens |first19=Ian R. |last20=Vreux |first20=Jean-Marie |last21=Zorec|first21=Jean |display-authors=6 |year=2000|doi=10.1046/j.1365-8711.2000.03542.x|doi-access=free}}</ref><ref name="aass34_1" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[남십자자리 카파 (항성)|남십자자리 카파]] ([[센타우루스자리 OB1]]의 [[보석상자 성단]]에 존재)
|23
|7,500
| style="background:lightblue;color:darkblue;" |'''5.98'''
|16,300
|항성진화 모델
|{{SIMBAD link|Kappa+Crucis|SIMBAD}}
|<ref>{{저널 인용|last1=Dufton|first1=P.L. |last2=Smartt|first2=S.J. |last3=Lee |first3=J.K. |last4=Ryans |first4=R.S.I. |last5=Hunter |first5=I. |last6=Evans|first6=C.J. |last7=Herrero |first7=A. |last8=Trundle|first8=C.|last9=Lennon |first9=D.J. |last10=Irwin |first10=M.J. |last11=Kaufer |first11=A. |display-authors=6 |date=2006|title=The VLT-FLAMES survey of massive stars: stellar parameters and rotational velocities in NGC 3293, NGC 4755 and NGC 6611|journal=Astronomy & Astrophysics|volume=457|issue=1 |pages=265–280 |arxiv=astro-ph/0606409|bibcode=2006A&A...457..265D|doi=10.1051/0004-6361:20065392|s2cid=15874925|issn=0004-6361}}</ref><ref name="tycho2" />
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[WR 78]] ([[전갈자리 OB1 성협|전갈자리 OB1]]의 [[NGC 6231]]에 존재)
|22
| 4,100
| style="background:lightblue;color:darkblue;" |'''6.48'''
|50,100
|분광법
|{{SIMBAD link|WR+78|SIMBAD}}
|<ref name=hamann2019/><ref name=gcvs/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[큰개자리 오미크론2]] ([[콜린더 목록|콜린더 121]]에 존재)
|21.4
|2,800
| style="background:lightblue;color:darkblue;" |'''3.043'''
|15,500
|항성진화 모델
|{{SIMBAD link|Omicron2+Canis+Majoris|SIMBAD}}
|<ref name=tetzlaff/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[리겔]] A ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|21
|860
| style="background:lightblue;color:darkblue;" |'''0.13'''
|12,100
|항성진화 모델
|{{SIMBAD link|Beta+Orionis+A|SIMBAD}}
|<ref name=schultz>{{저널 인용 |last1=Shultz |first1=M. |last2=Wade |first2=G.A. |last3=Petit |first3=V. |last4=Grunhut |first4=J. |last5=Neiner |first5=C. |last6=Hanes |first6=D. |collaboration=MiMeS Collaboration |year=2014 |title=An observational evaluation of magnetic confinement in the winds of BA supergiants |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=438 |issue=2 |page=1114 |doi=10.1093/mnras/stt2260 |s2cid=118557626 |bibcode=2014MNRAS.438.1114S |arxiv=1311.5116}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[알루드라]] ([[콜린더 목록|콜린더 121]]에 존재)
|21
|2,000
| style="background:lightblue;color:darkblue;" |'''2.45'''
|15,000
|항성진화 모델
|{{SIMBAD link|Eta+Canis+Majoris|SIMBAD}}
|<ref name="Searle 20082" /><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[땅꾼자리 제타]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[전갈자리-센타우루스자리 성협|상부 전갈자리 성협]]에 존재)
|20.2
|370
| style="background:lightblue;color:darkblue;" |'''2.569'''
|34,000
|항성진화 모델
|{{SIMBAD link|Zeta+Ophiuchi|SIMBAD}}
|<ref name="repolust"/><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[오리온자리 웁실론]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|20
|2,900
| style="background:lightblue;color:darkblue;" |'''4.618'''
|33,400
|항성진화 모델
|{{SIMBAD link|Upsilon+Orionis|SIMBAD}}
|<ref>{{저널 인용 |last=Smith |first=M.A. |date=August 1981 |title=Nonradial pulsations in the zero-age main-sequence star upsilon Orionis /09.5 V/ |journal=[[The Astrophysical Journal]] |lang=en |volume=248 |pages=214–221 |bibcode=1981ApJ...248..214S |doi=10.1086/159145 |issn=0004-637X}}</ref><ref>{{저널 인용 |last=Nieva|first=M.-F. |date=2013 |title=Temperature, gravity, and bolometric correction scales for non-supergiant OB stars |journal=Astronomy & Astrophysics|volume=550 |page=A26 |arxiv=1212.0928 |bibcode=2013A&A...550A..26N |doi=10.1051/0004-6361/201219677 |s2cid=119275940 |issn=0004-6361}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[오리온자리 시그마]] Aa ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|18
|1,260
| style="background:lightblue;color:darkblue;" |'''4.07'''<br/>{{small|(연성계 전체)}}
|35,000
|분광법
|{{SIMBAD link|Sigma+Orionis+A|SIMBAD}}
|<ref name="simondiaz2015">{{저널 인용 |last1=Simón-Díaz |first1=S. |last2=Caballero |first2=J.A. |last3=Lorenzo |first3=J. |last4=Maíz Apellániz |first4=J. |last5=Schneider |first5=F.R.N. |last6=Negueruela |first6=I. |last7=Barbá |first7=R.H. |last8=Dorda |first8=R.|last9=Marco |first9=A. |last10=Montes |first10=D.|last11=Pellerin|first11=A.|last12=Sanchez-Bermudez |first12=J. |last13=Sódor |first13=Á. |last14=Sota |first14=A. |display-authors=6 |year=2015 |title=Orbital and Physical Properties of the σ Ori Aa, Ab, B Triple System |journal=[[The Astrophysical Journal]] |volume=799 |issue=2 |page=169 |bibcode=2015ApJ...799..169S |arxiv=1412.3469 |doi=10.1088/0004-637X/799/2/169|s2cid=118500350}}</ref><ref name="wds">{{저널 인용 |last1=Mason |first1=Brian D. |last2=Wycoff |first2=Gary L. |last3=Hartkopf |first3=William I. |last4=Douglass |first4=Geoffrey G. |last5=Worley |first5=Charles E. |year=2001 |title=The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog |journal=[[The Astronomical Journal]] |volume=122 |issue=6 |page=3466 |doi=10.1086/323920 |doi-access=free |bibcode=2001AJ....122.3466M}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[비둘기자리 뮤]] ([[사다리꼴성단]]에 존재하는 [[폭주성]])
|16
|1,300
| style="background:lightblue;color:darkblue;" |'''5.18'''
|33,000
|분광법
|{{SIMBAD link|mu+Columbae|SIMBAD}}
|<ref name=Martins2005>{{저널 인용|last1=Martins|first1=F.|last2=Schaerer|first2=D.|last3=Hillier|first3=D. J.|last4=Meynadier|first4=F.|last5=Heydari-Malayeri |first5=M.|last6=Walborn|first6=N. R.|date=2005 |title=O stars with weak winds: the Galactic case |journal=Astronomy & Astrophysics |volume=441 |issue=2 |pages=735–762 |arxiv=astro-ph/0507278 |bibcode=2005A&A...441..735M|doi=10.1051/0004-6361:20052927|s2cid=11547293|issn=0004-6361}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[사이프]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|15.5
|650
| style="background:lightblue;color:darkblue;" |'''2.09'''
|26,500
|항성진화 모델
|{{SIMBAD link|Kappa+Orionis|SIMBAD}}
|<ref name=an331_4_3492>{{저널 인용 |last1=Hohle |first1=M.M. |last2=Neuhäuser |first2=R. |last3=Schutz |first3=B.F. |date=April 2010 |title=Masses and luminosities of O- and B-type stars and red supergiants |journal=Astronomische Nachrichten |volume=331 |issue=4 |page=349 |arxiv=1003.2335 |bibcode=2010AN....331..349H |doi=10.1002/asna.200911355 |s2cid=111387483}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[백조자리 시그마]] ([[백조자리 OB4]]에 존재)
|15
|3,260
| style="background:lightblue;color:darkblue;" |'''4.233'''
|10,800
|항성진화 모델
|{{SIMBAD link|Sigma+Cygni|SIMBAD}}
|<ref name=przybilla>{{저널 인용 |last1=Przybilla |first1=N. |last2=Firnstein |first2=M. |last3=Nieva |first3=M.F. |last4=Meynet |first4=G. |last5=Maeder |first5=A. |year=2010 |title=Mixing of CNO-cycled matter in massive stars|journal=Astronomy and Astrophysics|volume=517 |page=A38 |bibcode=2010A&A...517A..38P |arxiv=1005.2278 |doi=10.1051/0004-6361/201014164 |s2cid=55532189}}</ref><ref name="firnstein">{{저널 인용 |last1=Firnstein |first1=M. |last2=Przybilla |first2=N. |year=2012 |title=Quantitative spectroscopy of Galactic BA-type supergiants. I. Atmospheric parameters |journal=[[Astronomy & Astrophysics]] |volume=543 |page=A80 |arxiv=1207.0308 |bibcode=2012A&A...543A..80F |doi=10.1051/0004-6361/201219034 |s2cid=54725386}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[용골자리 세타]] A ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[IC 2602]]에 존재)
|14.9
|460
| style="background:lightblue;color:darkblue;" |'''2.76'''<br/>{{small|(연성계 전체)}}
|31,000
|항성진화 모델
|{{SIMBAD link|Theta+Carinae|SIMBAD}}
|<ref name=tetzlaff/><ref name=clpl4/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[오리온자리 세타2]] B ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|14.8
|1,500
| style="background:lightblue;color:darkblue;" |'''6.38'''
|29,300
|분광법
|{{SIMBAD link|Theta2+Orionis+B|SIMBAD}}
|<ref name="nieva">{{저널 인용 |last1=Nieva |first1=María-Fernanda |last2=Przybilla |first2=Norbert |year=2014 |title=Fundamental properties of nearby single early B-type stars |journal=Astronomy & Astrophysics |volume=566 |page=A7 |bibcode=2014A&A...566A...7N |arxiv=1412.1418 |doi=10.1051/0004-6361/201423373 |s2cid=119227033}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[페르세우스자리 제타]] ([[페르세우스자리 OB2]]에 존재)
|14.5
|750
| style="background:lightblue;color:darkblue;" |'''2.86'''
|20,800
|항성진화 모델
|{{SIMBAD link|Zeta+Persei|SIMBAD}}
|<ref name=an331_4_3492/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[오리온자리 시그마]] B ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재)
|14
|1,260
| style="background:lightblue;color:darkblue;" |'''4.07'''<br/>{{small|(연성계 전체)}}
|31,000
|분광법
|{{SIMBAD link|Sigma+Orionis+B|SIMBAD}}
|<ref name=simondiaz2015/><ref name=wds/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[미르잠]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[국부 거품]]에 존재)
|13.5
|490
| style="background:lightblue;color:darkblue;" |'''1.985'''
|23,200
|항성진화 모델
|{{SIMBAD link|Beta+Canis+Majoris|SIMBAD}}
|<ref name=aaa459_2_589>{{저널 인용 | last1=Mazumdar | first1=A. | last2=Briquet | first2=M. | last3=Desmet | first3=M. | last4=Aerts | first4=C. | title=An asteroseismic study of the β Cephei star β Canis Majoris | journal=Astronomy and Astrophysics | volume=459 | issue=2 | pages=589–596 |date=November 2006 | doi=10.1051/0004-6361:20064980 | bibcode=2006A&A...459..589M |arxiv = astro-ph/0607261 | s2cid=11807580 }}</ref><ref name="mnassa31_69">{{저널 인용 | last1=Cousins | first1=A.W.J. | year=1972 | title=UBV Photometry of Some Very Bright Stars | journal=Monthly Notes of the Astronomical Society of Southern Africa | volume=31 | page=69 | bibcode=1972MNSSA..31...69C }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[페르세우스자리 엡실론]] A ([[페르세우스자리 알파 성단]]에 존재)
|13.5
|640
| style="background:lightblue;color:darkblue;" |'''2.88'''<br/>{{small|(연성계 전체)}}
|26,500
|항성진화 모델
|{{SIMBAD link|Epsilon+Persei|SIMBAD}}
|<ref name=aaa446_2_583>{{저널 인용 | last1=Libich | first1=J. | last2=Harmanec | first2=P. | last3=Vondrák | first3=J. | last4=Yang | first4=S. | last5=Hadrava | first5=P. | last6=Aerts | first6=C. | last7=de Cat | first7=P. | last8=Koubský | first8=P. | last9=Škoda | first9=P. | display-authors=6 |date=February 2006 | title=The new orbital elements and properties of ɛ Persei | journal=Astronomy and Astrophysics | volume=446 | issue=2 | pages=583–589 | doi=10.1051/0004-6361:20053032 | bibcode=2006A&A...446..583L | doi-access=free | hdl=2066/35168 | hdl-access=free }}</ref><ref name="aj82_431">{{저널 인용 | last1=Lutz | first1=T.E. | last2=Lutz | first2=J.H. | author2-link=Julie Lutz | date=June 1977 | title=Spectral classification and UBV photometry of bright visual double stars | journal=Astronomical Journal | volume=82 | pages=431–434 | doi=10.1086/112066 | bibcode=1977AJ.....82..431L | doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[하트샤]] Aa2 ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[NGC 1980]]에 존재)
|13.1
|1,340
| style="background:lightblue;color:darkblue;" |'''2.77'''<br/>{{small|(연성계 전체)}}
|27,000
|항성진화 모델
|{{SIMBAD link|Iota+Orionis|SIMBAD}}
|<ref name=marchenko/><ref name=aass34_1/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[드슈바]] A ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[전갈자리-센타우루스자리 성협|상부 전갈자리 성협]]에 존재)
|13
|440
| style="background:lightblue;color:darkblue;" |'''2.307'''<br/>{{small|(연성계 전체)}}
|27,400
|항성진화 모델
|{{SIMBAD link|Delta+Scorpii|SIMBAD}}
|<ref name=miro>{{저널 인용 |last1=Miroshnichenko|first1=A.S. |last2=Pasechnik |first2=A.V. |last3=Manset |first3=N. |last4=Carciofi |first4=A.C. |last5=Rivinius |first5=Th. |last6=Štefl |first6=S. |last7=Gvaramadze |first7=V.V. |last8=Ribeiro |first8=J.|last9=Fernando|first9=A. |last10=Garrel |first10=T. |last11=Knapen|first11=J.H. |last12=Buil |first12=C. |last13=Heathcote |first13=B. |last14=Pollmann|first14=E. |last15=Mauclaire |first15=B. |last16=Thizy |first16=O. |last17=Martin |first17=J. |last18=Zharikov |first18=S.V. |last19=Okazaki |first19=A.T. |last20=Gandet |first20=T.L. |last21=Eversberg |first21=T. |last22=Reinecke |first22=N. |display-authors=6 |year=2013 |title=The 2011 periastron passage of the Be binary δ Scorpii |journal=[[The Astrophysical Journal]] |volume=766 |issue=2 |page=119 |doi=10.1088/0004-637X/766/2/119 |bibcode=2013ApJ...766..119M |arxiv = 1302.4021 |s2cid=38692193}}</ref><ref>{{저널 인용 |last1=Gutierrez-Moreno |first1=Adelina |last2=Moreno |first2=Hugo |date=1968-06-01 |title=A Photometric Investigation of the SCORPlO-CENTAURUS Association |journal=The Astrophysical Journal Supplement Series |volume=15 |page=459 |bibcode=1968ApJS...15..459G |doi=10.1086/190168 |issn=0067-0049|doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|O}};text-align:left;" | [[오리온자리 시그마]] Ab [[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[오리온자리 OB1 성협|오리온자리 OB1]]에 존재
|13
|1,260
| style="background:lightblue;color:darkblue;" |'''4.07'''<br/>{{small|(연성계 전체)}}
|29,000
|분광법
|{{SIMBAD link|Sigma+Orionis+A|SIMBAD}}
|<ref name=simondiaz2015/><ref name=wds/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[파리자리 세타]] Aa ([[센타우루스자리 OB1]]에 존재하는 WR 48)
|11.5
|7,400
| style="background:lightblue;color:darkblue;" |'''5.53'''<br/>{{small|(연성계 전체)}}
|83,000
|분광법
|{{SIMBAD link|Theta+Muscae+A|SIMBAD}}
|<ref name="nugis">{{저널 인용 |last1=Nugis |first1=T. |last2=Lamers |first2=H.J.G.L.M. |year=2000 |title=Mass-loss rates of Wolf-Rayet stars as a function of stellar parameters |journal=[[Astronomy and Astrophysics]] |volume=360 |page=227 |bibcode=2000A&A...360..227N}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|WC}};text-align:left;" | [[돛자리 감마|돛자리 감마2]] A ([[돛자리 OB2]]에 존재하는 WR 11)
|9
|1,230
| style="background:lightblue;color:darkblue;" |'''1.83'''<br/>{{small|(연성계 전체)}}
|57,000
|분광법
|{{SIMBAD link|Gamma2+Velorum|SIMBAD}}
|<ref name="GammaVelorum">{{저널 인용 |last1=North |first1=J.R. |last2=Tuthill |first2=P.G. |last3=Tango |first3=W.J. |last4=Davis |first4=J. |date=2007-05-01 |title=γ2 Velorum: Orbital solution and fundamental parameter determination with SUSI |journal=Monthly Notices of the Royal Astronomical Society |lang=en |volume=377|issue=1 |pages=415–424 |arxiv=astro-ph/0702375 |bibcode=2007MNRAS.377..415N |doi=10.1111/j.1365-2966.2007.11608.x |s2cid=16425744 |issn=0035-8711}}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[땅꾼자리 로]] A  ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[땅군자리 로 분자운 복합체]]에 존재)
|8.7
|360
| style="background:lightblue;color:darkblue;" |'''4.63'''<br/>{{small|(연성계 전체)}}
|22,000
|항성진화 모델
|{{SIMBAD link|Rho+Ophiuchi+A|SIMBAD}}
|<ref name=tetzlaff/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[벨라트릭스]] ([[오리온자리 분자운 복합체|오리온자리 복합체]]의 [[벨라트릭스|벨라트릭스 성단]]에 존재)
|7.7
|250
| style="background:lightblue;color:darkblue;" | '''1.64'''
|21,800
|항성진화 모델
|{{SIMBAD link|Gamma+Orionis|SIMBAD}}
|<ref name="challouf2">{{저널 인용 |last1=Challouf |first1=M. |last2=Nardetto |first2=N.|last3=Mourard|first3=D.|last4=Graczyk |first4=D. |last5=Aroui |first5=H. |last6=Chesneau |first6=O. |last7=Delaa |first7=O. |last8=Pietrzyński |first8=G. |last9=Gieren |first9=W. |last10=Ligi |first10=R. |last11=Meilland |first11=A. |last12=Perraut |first12=K. |last13=Tallon-Bosc |first13=I. |last14=McAlister |first14=H. |last15=ten&nbsp;Brummelaar |first15=T. |first16=J. |last16=Sturmann |last17=Sturmann |first17=L. |last18=Turner |first18=N. |last19=Farrington |first19=C. |last20=Vargas |first20=N. |last21=Scott |first21=N. |display-authors=6 |year=2014 |title=Improving the surface brightness-color relation for early-type stars using optical interferometry |journal=[[Astronomy & Astrophysics]] |volume=570 |page=A104 |arxiv=1409.1351 |bibcode=2014A&A...570A.104C |doi=10.1051/0004-6361/201423772 |s2cid=14624307}}</ref><ref name=ducati/>
|- style="text-align:center;"
|style="background: {{항성-색깔|B}};text-align:left;" | [[안타레스]] B ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[루프 I 거품]]에 존재)
|7.2
|550
| style="background:lightblue;color:darkblue;" |'''5.5'''
|18,500
|항성진화 모델
|{{SIMBAD link|Alpha+Scorpii+B|SIMBAD}}
|<ref name=antaresb>{{저널 인용 |last1=Kudritzki |first1=R.P. |last2=Reimers |first2=D. |date=1978 |title=On the absolute scale of mass-loss in red giants. II. Circumstellar absorption lines in the spectrum of {{nobr|α Sco B}} and mass-loss of {{nobr|α Sco A}} |journal=Astronomy and Astrophysics |volume=70 |page=227 |bibcode=1978A&A....70..227K}}</ref><ref name=hr/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[황소자리 람다]] A ([[물고기자리-에리다누스자리 성류]]에 존재)
|7.18
|480
| style="background:lightblue;color:darkblue;" | '''3.47'''<br/>{{small|(연성계 전체)}}
|18,700
|항성진화 모델
|{{SIMBAD link|Lambda+Tauri|SIMBAD}}
|<ref name=mnras406_2_1071>{{저널 인용 | last1=Dervişoğlu | first1=A. | last2=Tout | first2=Christopher A. | last3=Ibanoğlu | first3=C. |date=August 2010 | title=Spin angular momentum evolution of the long-period Algols | journal=Monthly Notices of the Royal Astronomical Society | volume=406 | issue=2 | pages=1071–1083 | doi=10.1111/j.1365-2966.2010.16732.x | bibcode=2010MNRAS.406.1071D |arxiv = 1003.4392 | s2cid=119198387 }}</ref><ref name="aaass34_1">{{저널 인용 | last1=Nicolet | first1=B. | title=Catalogue of homogeneous data in the UBV photoelectric photometric system | journal=Astronomy and Astrophysics Supplement Series | volume=34 | pages=1–49 |date=October 1978 | bibcode=1978A&AS...34....1N }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[페르세우스자리 델타]] ([[페르세우스자리 알파 성단]]에 존재)
|7
|520
| style="background:lightblue;color:darkblue;" |'''3.01'''
|14,900
|항성진화 모델
|{{SIMBAD link|Delta+Persei|SIMBAD}}
|<ref name=tetzlaff/><ref name=clpl4/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[페르세우스자리 프시]] ([[페르세우스자리 알파 성단]]에 존재)
|6.2
|580
| style="background:lightblue;color:darkblue;" |'''4.31'''
|16,000
|항성진화 모델
|{{SIMBAD link|Psi+Persei|SIMBAD}}
|<ref name=tetzlaff/><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" |[[피콕 (항성)]] Aa ([[큰부리새자리-시계자리 성협]]에 존재)
|5.91
|180
| style="background:lightblue;color:darkblue;" |'''1.94'''
|17,700
|항성진화 모델
|{{SIMBAD link|Alpha+Pavonis|SIMBAD}}
|<ref name=david>{{저널 인용 |last1=David |first1=Trevor J. |last2=Hillenbrand |first2=Lynne A. |year=2015 |title=The ages of early-type stars: Strömgren photometric methods calibrated, validated, tested, and applied to hosts and prospective hosts of directly imaged exoplanets |journal=[[The Astrophysical Journal]] |volume=804 |issue=2 |page=146 |bibcode=2015ApJ...804..146D |arxiv=1501.03154 |doi=10.1088/0004-637X/804/2/146 |s2cid=33401607}}</ref><ref name="aass34_1">{{저널 인용 | last1=Nicolet | first1=B. | year=1978 | title=Photoelectric photometric Catalogue of homogeneous measurements in the UBV System | journal=Astronomy and Astrophysics Supplement Series | volume=34 | pages=1–49 | bibcode=1978A&AS...34....1N }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[알키오네 (항성)]] A ([[플레이아데스 성단]]에 존재)
|5.9
|440
| style="background:lightblue;color:darkblue;" |'''2.87'''<br/>{{small|(연성계 전체)}}
|12,300
|항성진화 모델
|{{SIMBAD link|Eta+Tauri|SIMBAD}}
|<ref name=zorec>{{저널 인용 |last1=Zorec |first1=J. |last2=Frémat |first2=Y. |last3=Cidale |first3=L. |year=2005 |title=On the evolutionary status of Be stars. I. Field Be stars near the Sun |journal=Astronomy and Astrophysics |volume=441 |issue=1 |pages=235–248 |doi=10.1051/0004-6361:20053051 |bibcode=2005A&A...441..235Z |arxiv = astro-ph/0509119 |s2cid=17592657}}</ref><ref name="ducati" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[뮬리파인]] ([[콜린더 목록|콜린더 121]]에 존재)
|5.6
|440
| style="background:lightblue;color:darkblue;" |'''4.1'''
|13,600
|항성진화 모델
|{{SIMBAD link|Gamma+Canis+Majoris|SIMBAD}}
|<ref name=tetzlaff/><ref name=apjss52_7>{{저널 인용 | last1=Fernie | first1=J.D. | title=New UBVRI photometry for 900&nbsp;supergiants | journal=Astrophysical Journal Supplement Series | volume=52 | pages=7–22 | date=May 1983 | doi=10.1086/190856 | bibcode=1983ApJS...52....7F | doi-access=free }}</ref>
|- style="text-align:center;"
|style="background: {{항성-색깔|B}};text-align:left;" | [[돛자리 오미크론]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[IC 2391]]에 존재)
|5.5
|490
|style="background:lightblue;color:darkblue;"| '''3.6'''
|16,200
|항성진화 모델
|{{SIMBAD link|Omicron+Velorum|SIMBAD}}
|<ref>{{저널 인용 |last1=Hubrig |first1=S. |last2=Briquet |first2=M. |last3=de&nbsp;Cat |first3=P. |last4=Schöller |first4=M. |last5=Morel|first5=T. |last6=Ilyin |first6=I. |date=2009 |title=New magnetic field measurements of β&nbsp;Cephei stars and slowly pulsating B stars |journal=Astronomische Nachrichten |language=en |volume=330 |issue=4 |pages=317–329 |arxiv=0902.1314 |bibcode=2009AN....330..317H |doi=10.1002/asna.200811187 |s2cid=17497112}}</ref><ref name=clpl4>{{저널 인용 | last1=Johnson | first1=H.L. | last2=Iriarte | first2=B. | last3=Mitchell | first3=R.I. | last4=Wisniewskj | first4=W.Z. | year=1966 | title=UBVRIJKL photometry of the bright stars | journal=Communications of the Lunar and Planetary Laboratory | volume=4 | issue=99 | page=99 | bibcode=1966CoLPL...4...99J }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[물병자리 오미크론]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|4.2
|440
| style="background:lightblue;color:darkblue;" |'''4.71'''
|13,500
|항성진화 모델
|{{SIMBAD link|Omicron+Aquarii|SIMBAD}}
|<ref name=deAlmeida_et_al_2020>{{저널 인용 | title=Visible and near-infrared spectro-interferometric analysis of the edge-on Be star o Aquarii | last1=de Almeida | first1=E.S.G. | last2=Meilland | first2=A. | last3=Domiciano de Souza | first3=A. | last4=Stee | first4=P. | last5=Mourard | first5=D. | last6=Nardetto | first6=N. | last7=Ligi | first7=R. | last8=Tallon-Bosc | first8=I. | last9=Faes | first9=D.M. | last10=Carciofi | first10=A.C. | last11=Bednarski | first11=D. | last12=Mota | first12=B.C. | last13=Turner | first13=N. | last14=ten&nbsp;Brummelaar | first14=T.A. | display-authors=6 | date=April 2020 | journal=Astronomy & Astrophysics | volume=636 | id=A110 | page=23 | doi=10.1051/0004-6361/201936039 | arxiv=2002.09552 | bibcode=2020A&A...636A.110D | s2cid=211258993 }}</ref><ref name=aj84_1713>{{저널 인용 | last1=Feinstein | first1=A. | last2=Marraco | first2=H.G. | date=November 1979 | title=The photometric behavior of Be Stars | journal=Astronomical Journal | volume=84 | pages=1713–1725 | doi=10.1086/112600 | bibcode=1979AJ.....84.1713F| doi-access=free }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[화로자리 누]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|3.65
|370
| style="background:lightblue;color:darkblue;" |'''4.69'''
|13,400
|항성진화 모델
|{{SIMBAD link|nu+Fornacis|SIMBAD}}
|<ref name=aaa334_181>{{저널 인용 | last1=North | first1=P. | title=Do SI stars undergo any rotational braking? | journal=Astronomy and Astrophysics | volume=334 | pages=181–187 | date=1998 | bibcode=1998A&A...334..181N | arxiv=astro-ph/9802286 }}</ref><ref name=ducati/>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[에리다누스자리 피]] ([[큰부리새자리-시계자리 성협]]에 존재)
|3.55
|150
| style="background:lightblue;color:darkblue;" |'''3.55'''
|13,700
|항성진화 모델
|{{SIMBAD link|Phi+Eridani|SIMBAD}}
|<ref name=david/><ref name=Mermilliod1986>{{보고서 인용 | last1=Mermilliod | first1=J.-C. | year=1986 | title=Compilation of Eggen's UBV data, transformed to UBV (unpublished) | journal=Catalogue of Eggen's UBV Data | publisher=[[SIMBAD]] | bibcode=1986EgUBV........0M }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[카멜레온자리 에타]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[카멜레온자리 에타 운동성단]]에 존재)
|3.2
|310
| style="background:lightblue;color:darkblue;" |'''5.453'''
|12,500
|항성진화 모델
|{{SIMBAD link|Eta+Chamaeleontis|SIMBAD}}
|<ref name=Mamajek>{{저널 인용 |author1=Mamajek, Eric E. |author2=Lawson, Warrick A. |author3=Feigelson, Eric D. |year=1999 |title=The η&nbsp;Chamaeleontis cluster: A remarkable new nearby young open cluster |journal=The Astrophysical Journal |volume=516 |issue=2 |pages=L77–L80 |bibcode=1999ApJ...516L..77M|doi=10.1086/312005|doi-access=free}}</ref><ref name="tycho2" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[카멜레온자리 엡실론]] ([[전갈자리-센타우루스자리 성협|전갈자리 OB2]]의 [[카멜레온자리 엡실론 운동성단]]에 존재)
|2.87
|360
| style="background:lightblue;color:darkblue;" |'''4.91'''
|10,900
|항성진화 모델
|{{SIMBAD link|Epsilon+Chamaeleontis|SIMBAD}}
|<ref name="Fang2013">{{저널 인용 |last1=Fang|first1=M. |last2=van Boekel |first2=R. |last3=Bouwman|first3=J. |last4=Henning |first4=Th.|last5=Lawson |first5=W.A. |last6=Sicilia-Aguilar |first6=A. |date=January 2013 |title=Young stars in ϵ Chamaleontis and their disks: Disk evolution in sparse associations |journal=Astronomy & Astrophysics |volume=549 |page=A15 |arxiv=1209.5832 |bibcode=2013A&A...549A..15F |doi=10.1051/0004-6361/201118528|issn=0004-6361 |s2cid=118332644}}</ref><ref name="clpl4" />
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[물병자리 타우1]] ([[물고기자리-에리다누스자리 성류]]에 존재)
|2.68
|320
| style="background:lightblue;color:darkblue;" |'''5.66'''
|10,600
|항성진화 모델
|{{SIMBAD link|Tau1+Aquarii|SIMBAD}}
|<ref name=Zorec2012/><ref name="mnrassa27_11">{{저널 인용 | last1=Corben | first1=P.M. | last2=Stoy | first2=R.H. | title=Photoelectric Magnitudes and Colours for Bright Southern Stars | journal=Monthly Notes of the Astronomical Society of Southern Africa | volume=27 | page=11 | year=1968 | bibcode=1968MNSSA..27...11C}}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[물뱀자리 엡실론]] ([[큰부리새자리-시계자리 성협]]에 존재)
|2.64
|150
| style="background:lightblue;color:darkblue;" |'''4.12'''
|11,000
|항성진화 모델
|{{SIMBAD link|Epsilon+Hydri|SIMBAD}}
|<ref name=Zorec2012>{{저널 인용 | last1=Zorec | first1=J. | last2=Royer | first2=F. | year=2012 | title=Rotational velocities of A-type stars | journal=Astronomy & Astrophysics | volume=537 | page=A120 | s2cid=55586789 | arxiv=1201.2052 | bibcode=2012A&A...537A.120Z | doi=10.1051/0004-6361/201117691 }}</ref><ref name=XHIP>{{저널 인용 | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | year=2012 | title=XHIP: An extended hipparcos compilation | journal=Astronomy Letters | volume=38 | issue=5 | page=331 | s2cid=119257644 | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 }}</ref>
|- style="text-align:center;"
| style="background: {{항성-색깔|B}};text-align:left;" | [[큰부리새자리 베타]] ([[큰부리새자리-시계자리 성협]]에 존재)
|2.5
|140
| style="background:lightblue;color:darkblue;" |'''4.37'''
|10,600
|항성진화 모델
|{{SIMBAD link|Beta1+Tucanae|SIMBAD}}
|<ref name=tetzlaff/><ref name=hr/>
|- style="text-align:center;"
| style="background:lightyellow;text-align:left;" | [[태양]] ([[태양계]]에 존재)
|1
|0.0000158
| style="background:lightyellow;color:goldenrod;" |'''−26.744'''
|5,772
|표준
|{{URL | 1=https://www.iau.org/static/resolutions/IAU2015_English.pdf| 2=IAU}}
|<ref>{{저널 인용 |last1=Luzum |first1=Brian |last2=Capitaine |first2=Nicole |last3=Fienga |first3=Agnès |last4=Folkner |first4=William |last5=Fukushima |first5=Toshio |last6=Hilton |first6=James |last7=Hohenkerk |first7=Catherine |last8=Krasinsky |first8=George |last9=Petit |first9=Gérard |last10=Pitjeva |first10=Elena |last11=Soffel |first11=Michael |last12=Wallace |first12=Patrick |display-authors=6 |date=August 2011 |title=The IAU 2009 system of astronomical constants: the report of the IAU working group on numerical standards for Fundamental Astronomy |journal=Celestial Mechanics and Dynamical Astronomy |language=en |volume=110 |issue=4 |pages=293–304 |bibcode=2011CeMDA.110..293L |doi=10.1007/s10569-011-9352-4 |issn=0923-2958 |s2cid=122755461 |doi-access=free}}</ref><ref>{{저널 인용 |last1=Bessell |first1=M.S. |last2=Castelli |first2=F. |last3=Plez |first3=B. |date=May 1998 |title=Model atmospheres broad-band colors, bolometric corrections and temperature calibrations for O–M stars |journal=Astronomy & Astrophysics |volume=333 |pages=231–250 |bibcode=1998A&A...333..231B |issn=0004-6361 |s2cid=10513623}}</ref><ref>{{arXiv 인용 |last1=Mamajek |first1=E.E. |last2=Prsa |first2=A. |last3=Torres |first3=G. |last4=Harmanec |first4=P. |last5=Asplund |first5=M. |last6=Bennett |first6=P.D. |last7=Capitaine |first7=N. |last8=Christensen-Dalsgaard |first8=J. |last9=Depagne|first9=E. |last10=Folkner |first10=W.M. |last11=Haberreiter |first11=M. |first19=M.M. |first22=S.G. |last22=Stewart |first21=J. |last21=Schou |first20=M.T. |last20=Richards |first13=J.L. |last19=Montgomery |first18=E.F. |last18=Milone |first17=B.D. |last17=Mason |first16=J. |last16=Laskar |first15=D.W. |last15=Kurtz |first14=V. |last14=Kostov |last13=Hilton |first12=S. |last12=Hekker |display-authors=6 |date=October 2015 |title=IAU 2015 Resolution B3 on Recommended Nominal Conversion Constants for Selected Solar and Planetary Properties|eprint=1510.07674 |class=astro-ph.SR}}</ref>
|-
|}
{{각주|group=lower-alpha}}

==블랙홀==
{{본문|블랙홀|블랙홀 목록|질량이 큰 블랙홀 목록}}
[[블랙홀]]은 무거운 별의 진화의 종점이며 엄밀히 말하면 그들은 핵융합을 통해 더 이상 열과 빛을 생성하지 않기 때문에 별이 아니다. 일부 블랙홀은 우주론적 기원을 갖고 있을 수 있는데 그렇다면 결코 별이었던 적이 없을 것이며 이는 [[초대질량 블랙홀]]의 경우 특히 가능성이 높은 것으로 생각된다.

* [[항성질량 블랙홀]]은 약 4-15 {{태양질량|link=y}}인 물체다. 
* [[중간질량 블랙홀]]의 범위는 100-10,000 {{태양질량}}이다. 
* [[초대질량 블랙홀]]은 수백만 또는 수십억 {{태양질량}} 범위에 있다.

== 같이 보기 ==
{{cmn|colwidth=18em|
* [[가까운 별 목록]]
* [[갈색왜성 목록]]
* [[겉보기 등급순 별 목록]]
* [[광도 순 항성 목록]]
* [[극대거성]]
* [[반지름 순 별 목록]]
* [[밝은 청색변광성]]
* [[볼프-레이에별]]
* [[유효온도가 높은 항성 목록]]
* [[질량이 작은 별 목록]]
* [[초거성]]
* [[항성 목록]]
}}

== 각주 ==
{{각주|2}}

== 외부 링크 ==
* {{웹 인용 |url=http://hubblesite.org/newscenter/archive/releases/2005/05/ |title=Statistics in Arches cluster |website=HubbleSite |date=May 2005}}
* {{웹 인용 |url=http://www.space.com/scienceastronomy/070607_massive_star.html |title=Most Massive Star Discovered |website=Space.com|date=7 June 2007 }}
* {{웹 인용 |url=https://www.sciencedaily.com/releases/2005/03/050309142833.htm |title=Arches cluster |website=ScienceDaily |date=March 2005}}
* {{웹 인용 |title=How heavy can a star get? |url=http://www.3towers.com/sGrasslands/Essays/HeavyStar/HeavyStar01.asp |website=3towers |url-status=dead |archive-url=https://web.archive.org/web/20071028091902/http://www.3towers.com/sGrasslands/Essays/HeavyStar/HeavyStar01.asp |archive-date=2007-10-28}}
* {{웹 인용 |title=Hubble Unveils Monster Stars|url=https://www.nasa.gov/feature/goddard/2016/hubble-unveils-monster-stars |website=NASA |date=March 2016}}

{{항성}}
{{초신성}}
{{블랙홀}}

[[분류:항성 목록]]