Tarantula nebula
The Tarantula nebula (also known as 30 Doradus) is an H II region in the Large Magellanic Cloud (LMC). It was originally thought to be a star, but in 1751 Lacaille recognized it was a nebula.
The Tarantula nebula has an apparent magnitude of 8. Considering its distance of 49 kpc (160,000 light-years),[1] this is an extremely luminous object. Its luminosity is so great that if it were as close to Earth as the Orion Nebula, the Tarantula nebula would cast shadows.[2]
It is the most active starburst region known in the Local Group of galaxies. It is also one of the largest such regions in the Local Group with an estimated diameter of 200 pc.[3]
30 Doradus has at its centre the star cluster NGC 2070 which includes the group of stars known as R136.[4] This group puts out most of the energy that makes the nebula visible. The estimated mass of the cluster is 450,000 solar masses. It may become a globular cluster in the future.[5]
In addition to NGC 2070, the Tarantula nebula has other star clusters, including the much older Hodge 301. The most massive stars of Hodge 301 have already exploded in supernovae.[6] The closest supernova observed since the invention of the telescope,[7] Supernova 1987A, occurred in the outskirts of the Tarantula Nebula.[8] The remnants of many other supernovae are difficult to detect in the complex nebulosity.[9]
Tarantula Nebula Media
The brilliant stars in the Tarantula Nebula unleash a torrent of ultraviolet light and stellar winds that etch away at the hydrogen gas cloud in which the stars were born.
Hubble's high resolution view of the star-forming region of Tarantula Nebula and the R136 super star cluster at its center
Detail of RMC 136a, cluster NGC 2070
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References
- ↑ SEDS Students for the exploration and development of space
- ↑ "National Optical Astronomy Observatory Press Release: NEIGHBOR GALAXY CAUGHT STEALING STARS". www.noao.edu. Archived from the original on 2019-05-03. Retrieved 2019-02-15.
- ↑ Lebouteiller V. et al 2008. Chemical composition and mixing in giant H II regions: NGC 3603, 30 Doradus, and N66. The Astrophysical Journal 680 (1): 398–419.
- ↑ Massey P. & Hunter D. 1998 (1998). "Star formation in R136: a cluster of O3 stars revealed by Hubble Space Telescope spectroscopy". The Astrophysical Journal. 493 (1): 180–194. Bibcode:1998ApJ...493..180M. doi:10.1086/305126. S2CID 122670111.
- ↑ Bosch, Guillermo; Terlevich, Elena & Terlevich, Roberto 2009. (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.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ Grebel, Eva K. & Chu, You-Hua 2000 (2000). "Hubble Space Telescope Photometry of Hodge 301: An "Old" Star Cluster in 30 Doradus". Astronomical Journal. 119 (2): 787–799. arXiv:astro-ph/9910426. Bibcode:2000AJ....119..787G. doi:10.1086/301218. S2CID 118590210.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ "Tarantula Nebula's Cosmic Web a Thing of Beauty". SPACE.com. 2011-03-21. Retrieved 2011-03-26.
- ↑ "Encyclopedia of Space". Authors: Couper,Heather; Henbest, Nigel. Retrieved 2 January 2013.
- ↑ Lazendic J.S. et al 2003. (2003). "Supernova remnant candidates in the 30 Doradus nebula". The Astrophysical Journal. 596 (1): 287–298. Bibcode:2003ApJ...596..287L. doi:10.1086/377630. S2CID 123264251.