Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30831
DC Field | Value | Language |
---|---|---|
dc.contributor.author | TRAFICANTE, ALESSIO | en_US |
dc.contributor.author | Fuller, G. A. | en_US |
dc.contributor.author | Smith, R. J. | en_US |
dc.contributor.author | Billot, N. | en_US |
dc.contributor.author | Duarte-Cabral, A. | en_US |
dc.contributor.author | Peretto, N. | en_US |
dc.contributor.author | MOLINARI, Sergio | en_US |
dc.contributor.author | Pineda, J. E. | en_US |
dc.date.accessioned | 2021-04-21T13:38:31Z | - |
dc.date.available | 2021-04-21T13:38:31Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30831 | - |
dc.description.abstract | The dynamic activity in massive star-forming regions prior to the formation of bright protostars is still not fully investigated. In this work, we present observations of HCO<SUP>+</SUP> J = 1-0 and N<SUB>2</SUB>H<SUP>+</SUP> J = 1-0 made with the IRAM 30 m telescope towards a sample of 16 Herschel-identified massive 70 μm quiet clumps associated with infrared dark clouds. The clumps span a mass range from 300 to 2000 M<SUB>☉</SUB>. The N<SUB>2</SUB>H<SUP>+</SUP> data show that the regions have significant non-thermal motions with velocity dispersion between 0.28 and 1.5 km s<SUP>-1</SUP>, corresponding to Mach numbers between 2.6 and 11.5. The majority of the 70 μm quiet clumps have asymmetric HCO<SUP>+</SUP> line profiles, indicative of significant dynamical activity. We show that there is a correlation between the degree of line asymmetry and the surface density Σ of the clumps, with clumps of Σ ≳ 0.1 g cm<SUP>-2</SUP> having more asymmetric line profiles, and so are more dynamically active, than clumps with lower Σ. We explore the relationship between velocity dispersion, radius and Σ and show how it can be interpreted as a relationship between an acceleration generated by the gravitational field, a<SUB>G</SUB>, and the measured kinetic acceleration, a<SUB>k</SUB>, consistent with the majority of the non-thermal motions originating from self-gravity. Finally, we consider the role of external pressure and magnetic fields in the interplay of forces. | en_US |
dc.language.iso | eng | en_US |
dc.title | Massive 70 μm quiet clumps - II. Non-thermal motions driven by gravity in massive star formation? | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/stx2672 | en_US |
dc.identifier.scopus | 2-s2.0-85046085362 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/473/4/4975/4553529 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 473 | en_US |
dc.relation.issue | 4 | en_US |
dc.relation.firstpage | 4975 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | GBR | en_US |
dc.contributor.country | DEU | en_US |
dc.contributor.country | ESP | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018MNRAS.473.4975T | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.fulltext | With Fulltext | - |
item.grantfulltext | open | - |
item.languageiso639-1 | en | - |
item.openairetype | Article | - |
item.cerifentitytype | Publications | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.orcid | 0000-0003-1665-6402 | - |
crisitem.author.orcid | 0000-0002-9826-7525 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
Traficante_2018a.pdf | PDF editoriale | 1.35 MB | Adobe PDF | View/Open |
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