| DOI | Resolve DOI: https://doi.org/10.1051/0004-6361/201219423 |
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| Author | Search for: Minier, V.; Search for: Tremblin, P.; Search for: Hill, T.; Search for: Motte, F.; Search for: André, Ph.; Search for: Lo, N.; Search for: Schneider, N.; Search for: Audit, E.; Search for: White, G. J.; Search for: Hennemann, M.; Search for: Cunningham, M.; Search for: Deharveng, L.; Search for: Didelon, P.; Search for: Di Francesco, J.1; Search for: Elia, D.; Search for: Giannini, T.; Search for: Nguyen Luong, Q.; Search for: Pezzuto, S.; Search for: Rygl, K. L. J.; Search for: Spinoglio, L.; Search for: Ward-Thompson, D.; Search for: Zavagno, A. |
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| Affiliation | - National Research Council of Canada. National Science Infrastructure
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| Format | Text, Article |
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| Subject | Dynamical phenomena; Far-infrared; Filamentary structures; H II regions; HERSCHEL; Herschel space observatories; High-mass stars; ISM: individual objects; ISM: structure; Molecular clouds; Molecular lines; Natural evolution; Southern Hemisphere; Star formations; Stars: massive; Submillimetre; Galaxies; Hydrodynamics; Ionization; Morphology |
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| Abstract | Context. Ionising stars reshape their original molecular cloud and impact star formation, leading to spectacular morphologies such as bipolar nebulae around H ii regions. Molecular clouds are structured in filaments where stars principally form, as revealed by the Herschel space observatory. The prominent southern hemisphere H ii region, RCW 36, is one of these bipolar nebulae. Aims. We study the physical connection between the filamentary structures of the Vela C molecular cloud and the bipolar morphology of RCW 36, providing an in-depth view of the interplay occurring between ionisation and interstellar structures (bright-rims and pillars) around an H ii region. Methods. We have compared Herschel observations in five far-infrared and submillimetre filters with the PACS and SPIRE imagers, to dedicated numerical simulations and molecular line mapping. Results. Our results suggest that the RCW 36 bipolar morphology is a natural evolution of its filamentary beginnings under the impact of ionisation. Conclusions. Such results demonstrate that, filamentary structures can be the location of very dynamical phenomena inducing the formation of dense clumps at the edge of H ii regions. Moreover, these results could apply to better understanding the bipolar nebulae as a consequence of the expansion of an H ii region within a molecular ridge or an interstellar filament. |
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| Publication date | 2013-01-24 |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| NPARC number | 21270381 |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 86d757cd-9630-4598-9f48-b2308d30cb79 |
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| Record created | 2014-02-06 |
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| Record modified | 2020-04-22 |
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