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**R136**
R136
	In ultraviolet, visible, and red light by Hubble Space Telescope Wide Field Camera 3 ; Credit: NASA, ESA
Observation data (J2000.0 epoch)
Right ascension	05h 38m 42.396s
Declination	−69° 06′ 03.36″
Distance	157 kly (48.5 kpc)
Apparent magnitude (V)	9.50
Physical characteristics
Mass	90,000 M☉
Estimated age	1.5+0.3; −0.7 million years
Other designations	UCAC2 1803442, SAO 249329, HD 38268, TYC 9163-1014-1, CD-69 324, GC 7114
Associations
Constellation	Dorado
	See also: Open cluster, List of open clusters

R136 (formerly known as RMC 136 from the Radcliffe Observatory Magellanic Clouds catalogue^[4]) is the central concentration of stars in the NGC 2070 star cluster, which lies at the centre of the Tarantula Nebula in the Large Magellanic Cloud. When originally named it was an unresolved stellar object (catalogued as HD 38268 and Wolf-Rayet star Brey 82) but is now known to include 72 class O and Wolf–Rayet stars within 5 parsecs (20 arc seconds) of the centre of the cluster.^[5] The extreme number and concentration of young massive stars in this part of the LMC qualifies it as a starburst region.^[6]

Properties

R136 produces most of the energy that makes the Tarantula Nebula visible. The estimated mass of the cluster is 450,000 solar masses, suggesting it may become a globular cluster in the future.^[7] R136 has around 200 times the stellar density of a typical OB association such as Cygnus OB2.^[8] The central R136 concentration of the cluster is about 2 parsecs across, although the whole NGC 2070 cluster is much larger.^[8]

R136 is thought to be less than 2 million years old.^[8]^[9] None of the member stars are significantly evolved, and none are thought to have exploded as supernova. Because of this, the cluster contains no red supergiants, blue hypergiants, or luminous blue variables. The brightest stars are WNh, O supergiants, and OIf/WN slash stars, all extremely massive fully convective stars. A small number of B-type main sequence stars have been detected in the outskirts of the cluster, but less massive and less luminous stars cannot be resolved from the dense cluster core at the large distance of the LMC.^[5]

R136a

R136a is the bright knot at the centre of R136. It consists of eight extremely massive stars, three of them Wolf-Rayet stars and the rest early O-class stars.^[2]

Components

The cluster contains many of the most massive and luminous stars known, including R136a1. Within the central 5 parsecs there are 32 of the hottest type O stars (O2.0–3.5), 40 other O stars, and 12 Wolf-Rayet stars, mostly of the extremely luminous WNh type. Within 150 parsecs there are a further 325 O stars and 19Wolf-Rayet stars.^[5] Several runaway stars have been associated with R136, including VFTS 682.^[10] R136 was first resolved into three components R136a, R136b, and R136c. R136a was resolved using speckle interferometry and eventually space-based observations into as many as 24 components,^[11] dominated by R136a1, R136a2, and R136a3, all three being extremely massive WNh stars several million times more luminous than the sun.^[12]

Basic data for the original RMC 136 a, b, and c stars
Name	Right ascension^[5]	Declination^[5]	V^[2] (F555W)	Spectral type^[12]	M_V^[13] (F555W)	Temperature (K)^[12]^[14]	Luminosity (`L`_☉)^[12]^[14]	Mass (`M`_☉)^[12]^[14]
R136a1	05^h 38^m 42.39^s	−69° 06′ 02.91″	12.28	WN5h	−8.18	46,000	4,677,000	196
R136a2	05^h 38^m 42.40^s	−69° 06′ 02.88″	12.80	WN5h	−7.80	50,000	3,548,000	151
R136a3	05^h 38^m 42.33^s	−69° 06′ 03.27″	12.97	WN5h	−7.52	50,000	3,631,000	155
R136a4	05^h 38^m 42.34^s	−69° 06′ 02.60″	13.96	O3 V((f*))(n)	−6.68	50,000	1,905,000	108
R136a5	05^h 38^m 42.43^s	−69° 06′ 02.73″	13.71	O2I(n)f^*	−6.86	48,000	2,089,000	116
R136a6	05^h 38^m 42.29^s	−69° 06′ 03.37″	13.35	O2I(n)f^*p	−6.46	52,000	1,738,000	105
R136a7	05^h 38^m 42.41^s	−69° 06′ 02.57″	13.97	O3III(f^*)	−6.59	54,000	2,291,000	127
R136a8	05^h 38^m 42.37^s	−69° 06′ 01.9″?	14.42	O2–3V^[2]	−6.05^[2]	49,500	1,479,000	96
R136b	05^h 38^m 42.74^s	−69° 06′ 03.78″	13.24	O4If	−7.70	35,500	2,239,000	92
R136c	05^h 38^m 42.90^s	−69° 06′ 04.83″	12.86	WN5h^[15]	−7.9^[5]	42,170^[15]	3,802,000^[15]	142^[15]

Gallery

R136 observed with Hubble's WFC3^[16]
Runaway star speeding from 30 Doradus in an image taken by the Hubble Space Telescope
R136 in infrared (Hubble Space Telescope)

References

^ ^a ^b Høg, E.; Fabricius, C.; Makarov, V.V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (January 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars – Letter to the Editor". Astronomy and Astrophysics. 355: L27 – L30. Bibcode:2000A&A...355L..27H.
^ ^a ^b ^c ^d ^e ^f Crowther, Paul A.; Caballero-Nieves, S. M.; Bostroem, K. A.; Maíz Apellániz, J.; Schneider, F. R. N.; Walborn, N. R.; Angus, C. R.; Brott, I.; Bonanos, A.; De Koter, A.; De Mink, S. E.; Evans, C. J.; Gräfener, G.; Herrero, A.; Howarth, I. D.; Langer, N.; Lennon, D. J.; Puls, J.; Sana, H.; Vink, J. S. (2016). "The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of He II λ1640 in young star clusters". Monthly Notices of the Royal Astronomical Society. 458 (1): 624–659. arXiv:1603.04994. Bibcode:2016MNRAS.458..624C. doi:10.1093/mnras/stw273.
^ "RMC 136". SIMBAD. Centre de données astronomiques de Strasbourg.
^ Feast, M. W.; Thackeray, A. D.; Wesselink, A. J. (1960). "The brightest stars in the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society. 121 (4): 337. Bibcode:1960MNRAS.121..337F. doi:10.1093/mnras/121.4.337.
^ ^a ^b ^c ^d ^e ^f Doran, E. I.; Crowther, P. A.; de Koter, A.; Evans, C. J.; McEvoy, C.; Walborn, N. R.; Bastian, N.; Bestenlehner, J. M.; Grafener, G.; Herrero, A.; Kohler, K.; Maiz Apellaniz, J.; Najarro, F.; Puls, J.; Sana, H.; Schneider, F. R. N.; Taylor, W. D.; van Loon, J. Th.; Vink, J. S. (2013). "The VLT-FLAMES Tarantula Survey - XI. A census of the hot luminous stars and their feedback in 30 Doradus". Astronomy & Astrophysics. 558: A134. arXiv:1308.3412. Bibcode:2013A&A...558A.134D. doi:10.1051/0004-6361/201321824. S2CID 118510909.
^ Brandl, B.; Sams, B. J.; Bertoldi, F.; Eckart, A.; Genzel, R.; Drapatz, S.; Hofmann, R.; Loewe, M.; Quirrenbach, A. (1996). "Adaptive Optics Near-Infrared Imaging of R136 in 30 Doradus: The Stellar Population of a Nearby Starburst". The Astrophysical Journal. 466: 254. Bibcode:1996ApJ...466..254B. doi:10.1086/177507.
^ Bosch, Guillermo; Terlevich, Elena; Terlevich, Roberto (2009). "Gemini/GMOS Search for Massive Binaries in the Ionizing Cluster of 30 Dor". Astronomical Journal. 137 (2): 3437–3441. arXiv:0811.4748. Bibcode:2009AJ....137.3437B. doi:10.1088/0004-6256/137/2/3437. S2CID 17976455.
^ ^a ^b ^c Massey, P.; Hunter, D. A. (1998). "Star Formation in R136: A Cluster of O3 Stars Revealed by Hubble Space Telescope Spectroscopy". The Astrophysical Journal. 493 (1): 180. Bibcode:1998ApJ...493..180M. doi:10.1086/305126.
^ Crowther, P. A.; Schnurr, O.; Hirschi, R.; Yusof, N.; Parker, R. J.; Goodwin, S. P.; Kassim, H. A. (2010). "The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 M_⊙ stellar mass limit". Monthly Notices of the Royal Astronomical Society. 408 (2): 731. arXiv:1007.3284. Bibcode:2010MNRAS.408..731C. doi:10.1111/j.1365-2966.2010.17167.x. S2CID 53001712.
^ Banerjee, S.; Kroupa, P.; Oh, S. (2012). "Runaway massive stars from R136: Vfts 682 is very likely a "slow runaway"". The Astrophysical Journal. 746 (1): 15. arXiv:1111.0291. Bibcode:2012ApJ...746...15B. doi:10.1088/0004-637X/746/1/15. S2CID 117959362.
^ Campbell, B.; Hunter, D.A.; Holtzman, J.A.; Lauer, T.R.; Shayer, E.J.; Code, A.; et al. (November 1992). "Hubble Space Telescope Planetary Camera images of R136" (PDF). The Astronomical Journal. 104 (5): 1721–1742. Bibcode:1992AJ....104.1721C. doi:10.1086/116355.{{cite journal}}: CS1 maint: multiple names: authors list (link)
^ ^a ^b ^c ^d ^e Brands, S.; de Koter, A.; Bestenlehner, J.; Crowther, P. O; Sundqvist, J.; Puls, J.; Caballero-Nieves, S.; Abdul-Masih, M.; Driessen, F.; Garcia, M.; Geen, S.; Gräfener, G.; Hawcroft, C.; Kaper, L.; Keszthelyi, Z.; Langer, N.; Sana, H.; Schneider, Fabian R. N.; Shenar, T.; Vink, Jorick S. (7 April 2022). "The R136 star cluster dissected with Hubble Space Telescope/STIS. III. The most massive stars and their clumped winds". Astronomy & Astrophysics. 663: A36. arXiv:2202.11080. Bibcode:2022A&A...663A..36B. doi:10.1051/0004-6361/202142742. ISSN 0004-6361. S2CID 247025548.
^ Bestenlehner, Joachim M.; Crowther, Paul A.; Caballero-Nieves, Saida M.; Schneider, Fabian R. N.; Simón-Díaz, Sergio; Brands, Sarah A.; De Koter, Alex; Gräfener, Götz; Herrero, Artemio; Langer, Norbert; Lennon, Daniel J.; Maíz Apellániz, Jesus; Puls, Joachim; Vink, Jorick S. (2020). "The R136 star cluster dissected with Hubble Space Telescope/STIS. II. Physical properties of the most massive stars in R136". Monthly Notices of the Royal Astronomical Society. 499 (2): 1918. arXiv:2009.05136. Bibcode:2020MNRAS.499.1918B. doi:10.1093/mnras/staa2801.
^ ^a ^b ^c Kalari, Venu M.; Horch, Elliott P.; Salinas, Ricardo; Vink, Jorick S.; Andersen, Morten; Bestenlehner, Joachim M.; Rubio, Monica (26 July 2022). "Resolving the core of R136 in the optical". The Astrophysical Journal. 935 (2): 162. arXiv:2207.13078. Bibcode:2022ApJ...935..162K. doi:10.3847/1538-4357/ac8424. S2CID 251067072.
^ ^a ^b ^c ^d Schneider, F. R. N.; Sana, H.; Evans, C. J.; Bestenlehner, J. M.; Castro, N.; Fossati, L.; Gräfener, G.; Langer, N.; Ramírez-Agudelo, O. H.; Sabín-Sanjulián, C.; Simón-Díaz, S.; Tramper, F.; Crowther, P. A.; de Koter, A.; de Mink, S. E.; Dufton, P. L.; Garcia, M.; Gieles, M.; Hénault-Brunet, V.; Herrero, A.; Izzard, R. G.; Kalari, V.; Lennon, D. J.; Maíz Apellániz, J.; Markova, N.; Najarro, F.; Podsiadlowski, Ph.; Puls, J.; Taylor, W. D.; van Loon, J. Th.; Vink, J. S.; Norman, C. (2018). "An excess of massive stars in the local 30 Doradus starburst". Science. 359 (6371): 69–71. arXiv:1801.03107. Bibcode:2018Sci...359...69S. doi:10.1126/science.aan0106. PMID 29302009. S2CID 206658504.
^ NASA; ESA; Crowther, P. (17 March 2016). "R136 observed with WFC3". ESA/Hubble. Retrieved 23 March 2016.