Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/30830
DC Field | Value | Language |
---|---|---|
dc.contributor.author | TRAFICANTE, ALESSIO | en_US |
dc.contributor.author | Duarte-Cabral, A. | en_US |
dc.contributor.author | ELIA, Davide Quintino | en_US |
dc.contributor.author | Fuller, G. A. | en_US |
dc.contributor.author | Merello, M. | en_US |
dc.contributor.author | MOLINARI, Sergio | en_US |
dc.contributor.author | Peretto, N. | en_US |
dc.contributor.author | SCHISANO, EUGENIO | en_US |
dc.contributor.author | DI GIORGIO, Anna Maria | en_US |
dc.date.accessioned | 2021-04-21T13:36:12Z | - |
dc.date.available | 2021-04-21T13:36:12Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/30830 | - |
dc.description.abstract | We tested the validity of the three Larson relations in a sample of 213 massive clumps selected from the Herschel infrared Galactic Plane (Hi-GAL) survey, also using data from the Millimetre Astronomy Legacy Team 90 GHz (MALT90) survey of 3-mm emission lines. The clumps are divided into five evolutionary stages so that we can also discuss the Larson relations as a function of evolution. We show that this ensemble does not follow the three Larson relations, regardless of the clump's evolutionary phase. A consequence of this breakdown is that the dependence of the virial parameter α<SUB>vir</SUB> on mass (and radius) is only a function of the gravitational energy, independent of the kinetic energy of the system; thus, α<SUB>vir</SUB> is not a good descriptor of clump dynamics. Our results suggest that clumps with clear signatures of infall motions are statistically indistinguishable from clumps with no such signatures. The observed non-thermal motions are not necessarily ascribed to turbulence acting to sustain the gravity, but they might be a result of the gravitational collapse at the clump scales. This seems to be particularly true for the most massive (M ≥ 1000 M<SUB>☉</SUB>) clumps in the sample, where exceptionally high magnetic fields might not be enough to stabilize the collapse. | en_US |
dc.language.iso | eng | en_US |
dc.title | Testing the Larson relations in massive clumps | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/sty798 | en_US |
dc.identifier.scopus | 2-s2.0-85047124375 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/477/2/2220/4990719 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 477 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2220 | 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.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.477.2220T | 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.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.dept | IAPS Roma | - |
crisitem.author.orcid | 0000-0003-1665-6402 | - |
crisitem.author.orcid | 0000-0002-9120-5890 | - |
crisitem.author.orcid | 0000-0002-9826-7525 | - |
crisitem.author.orcid | 0000-0003-1560-3958 | - |
crisitem.author.orcid | 0000-0002-4767-2360 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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Traficante_2018b.pdf | PDF editoriale | 1.57 MB | Adobe PDF | View/Open |
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