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dc.contributor.author | Rizzo Caminos, José Ricardo | |
dc.contributor.author | Jiménez-Esteban, F. M. | |
dc.contributor.author | Ortiz, E. | |
dc.date.accessioned | 2016-07-26T18:05:53Z | |
dc.date.available | 2016-07-26T18:05:53Z | |
dc.date.issued | 2008 | |
dc.identifier.citation | Rizzo, J. R., Jiménez-Esteban, F. M., & Ortiz, E. (2008). Discovery of warm and dense molecular gas surrounding the ring nebula G79. 29+ 0.46. The Astrophysical Journal, 681(1), 355. | spa |
dc.identifier.issn | 0004637X | |
dc.identifier.issn | 15384357 | |
dc.identifier.uri | http://hdl.handle.net/11268/5474 | |
dc.description.abstract | We present for the first time the detection of mid-J CO line emission in the outskirts of an evolved massive star, which indicates the presence of warm and/or high-density molecular gas. Aiming to learn about the interplay between evolved massive stars and their surroundings, we have carried out CO J = 2→ 1, J = 3→ 2, and 13↑CO J = 2→ 1 line observations in a 4' × 4' field around the ring nebula G79.29+0.46, which is illuminated by a strong LBV star candidate. The whole field shows extended predominant emission in both CO and 13↑CO J = 2→ 1 lines, which probably comes from the large cloud which contains the star-forming region DR 15. When this large-scale emission is removed, minor-scale features become evident, particularly in the CO J = 3→ 2 line, strikingly coincident with the ring nebula. The high critical density of CO J = 3→ 2 (some 10↑4 cm↑−3) gives additional support for the association with the massive star, since high-density molecular gas has more chances to survive in such a harsh environment. This structure may have been produced by the cumulative effect of a strong steady wind in the LBV stage or earlier, which has compressed the surviving parent molecular cloud. In addition, immersed within this CO feature, we have also discovered a higher density clump (at least several ~10↑5 cm↑−3), unresolved by the telescope and probably having a higher kinetic temperature. Toward the clump, the presence of a jump of 14-16 km s↑−1 in the gas velocity may indicate the existence of a shock front. This clump may have been created by at least one mass eruption, 10↑3-10↑4 yr ago. Thus, this work shows that not all the molecular gas is destroyed during massive star evolution, and consequently we are dealing with a new laboratory where one can learn about the mass-loss phenomena associated to the brief LBV stage. | spa |
dc.description.sponsorship | Sin financiación | spa |
dc.language.iso | eng | spa |
dc.rights | Reconocimiento-NoComercial-CompartirIgual 3.0 | |
dc.rights.uri | http://creativecommons.org/licenses/by-nc-sa/3.0/es/ | |
dc.title | Discovery of warm and dense molecular gas surrounding the ring nebula G79.29+0.46 | spa |
dc.type | article | spa |
dc.description.impact | 6.331 JCR (2008) Q1, 6/48 Astronomy & astrophysics | spa |
dc.rights.accessRights | openAccess | spa |
dc.subject.uem | Dióxido de carbono-Aspectos ambientales | spa |
dc.subject.unesco | Astrofísica | spa |
dc.description.filiation | UEM | spa |
dc.peerreviewed | Si | spa |