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This process creates an enveloping nebula around the Wolf-Rayet star with a distinctive multi-ring structure. The nebula contains shells and cavities carved out by the stellar winds, surrounded by dense swept-up material. These structures become visible due to fluorescent emission from ionized gas as
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from Wolf-Rayet stars consist of streams of charged particles traveling at speeds of thousands of kilometers per second. These winds slam into the surrounding interstellar medium, generating shock waves that heat and ionize the gas and dust, causing it to glow and emit radiation in
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As a Wolf-Rayet star evolves and loses mass, its winds shape the surrounding gas and dust into bubble-like nebular structures. The inner region forms from the current stellar wind, while outer shells are remnants of previous mass-loss episodes.
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Wolf-Rayet stars represent a brief late stage in the evolution of some very massive stars. They have shed their outer hydrogen envelopes and their stellar winds now consist of heavier elements like helium, carbon, nitrogen, and oxygen.
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These nebulae exhibit intricate structures revealed in visible light as well as infrared, X-ray, and other wavelengths, providing insight into the powerful stellar winds and evolutionary processes around Wolf-Rayet stars.
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Eventually the star will shed more matter, ending its life in a spectacular supernova explosion that will dramatically alter the Wolf-Rayet nebula's structure and composition.
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Toalá, J. A.; Guerrero, M. A.; Ramos-Larios, G.; Guzmán, V. (2015). "WISE morphological study of Wolf-Rayet nebulae".
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S Zavala, J A Toalá, E Santamaría, G Ramos-Larios, L Sabin, J A Quino-Mendoza, G Rubio, M A Guerrero,
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3D mapping of the Wolf–Rayet nebula M 1-67: clues for post-common envelope evolution in massive stars
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249:, Volume 459, Issue 2, 21 June 2016, Pages 1505–1518, https://doi.org/10.1093/mnras/stw618
229:, Volume 513, Issue 3, July 2022, Pages 3317–3325, https://doi.org/10.1093/mnras/stac1097
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Helium stars: towards an understanding of Wolf–Rayet evolution
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247:Monthly Notices of the Royal Astronomical Society
227:Monthly Notices of the Royal Astronomical Society
37:is one of the highest-excitation nebulae in the
106:Some well-studied Wolf-Rayet nebulae include:
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65:. Wolf-Rayet stars are very hot, highly
16:Nebula which surrounds a Wolf–Rayet star
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241:L. A. S. McClelland, J. J. Eldridge,
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73:or heavier elements in their cores.
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26:is surrounded by a bubble nebula.
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41:, two satellite galaxies of the
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98:well as scattered starlight.
171:Astronomy & Astrophysics
380:Evaporating gaseous globule
201:10.1051/0004-6361/201525706
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193:2015A&A...578A..66T
140:Formation and evolution
416:Integrated Flux Nebula
119:(Thor's Helmet Nebula)
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406:Protoplanetary nebula
370:Giant molecular cloud
348:Protoplanetary nebula
131:(Nebula around WR 18)
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426:Post-stellar nebulae
517:Intergalactic blobs
482:High-velocity cloud
362:Pre-stellar nebulae
647:Wolf–Rayet nebulae
569:Supernova remnants
465:Interstellar cloud
444:Pulsar wind nebula
81:The strong, dense
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439:Supernova remnant
411:Wolf–Rayet nebula
338:Reflection nebula
321:Supernova remnant
113:(Crescent Nebula)
51:Wolf-Rayet nebula
39:Magellanic Clouds
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524:Lyman-alpha blob
434:Planetary nebula
316:Planetary nebula
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102:Notable examples
63:Wolf-Rayet stars
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552:Largest Nebulae
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508:Pinwheel nebula
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475:Infrared cirrus
470:Molecular cloud
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343:Variable nebula
311:Emission nebula
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77:Characteristics
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503:Bipolar nebula
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394:Stellar nebula
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306:Diffuse nebula
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83:stellar winds
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59:stellar winds
57:created from
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53:is a type of
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401:Nova remnant
385:Solar nebula
326:Nova remnant
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61:expelled by
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375:Bok globule
331:H II region
301:Dark nebula
92:wavelengths
641:Categories
625:Wiktionary
496:Morphology
487:H I region
449:Supershell
184:1503.06878
156:References
90:and other
557:Planetary
43:Milky Way
605:Category
209:55776698
129:NGC 3199
117:NGC 2359
111:NGC 6888
67:luminous
652:Nebulae
615:Commons
579:Related
547:Diffuse
287:Nebulae
189:Bibcode
177:: A66.
88:visible
571:(SNRs)
565:(PPNe)
458:Clouds
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71:helium
55:nebula
24:WR 31a
559:(PNe)
539:Lists
205:S2CID
179:arXiv
123:M1-67
197:doi
175:578
35:AB7
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49:A
279:e
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