Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/26692
DC Field | Value | Language |
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dc.contributor.author | MALDONADO PRADO, Jesus | en_US |
dc.contributor.author | Villaver, E. | en_US |
dc.date.accessioned | 2020-08-04T11:06:43Z | - |
dc.date.available | 2020-08-04T11:06:43Z | - |
dc.date.issued | 2017 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/26692 | - |
dc.description.abstract | Recent studies have shown that close-in brown dwarfs in the mass range 35-55 M$_{\rm Jup}$ are almost depleted as companions to stars, suggesting that objects with masses above and below this gap might have different formation mechanisms. We determine the fundamental stellar parameters, as well as individual abundances for a large sample of stars known to have a substellar companion in the brown dwarf regime. The sample is divided into stars hosting "massive" and "low-mass" brown dwarfs. Following previous works a threshold of 42.5 M$_{\rm Jup}$ was considered. Our results confirm that stars with brown dwarf companions do not follow the well-established gas-giant planet metallicity correlation seen in main-sequence planet hosts. Stars harbouring "massive" brown dwarfs show similar metallicity and abundance distribution as stars without known planets or with low-mass planets. We find a tendency of stars harbouring "less-massive" brown dwarfs of having slightly larger metallicity, [X$_{\rm Fe}$/Fe] values, and abundances of Sc II, Mn I, and Ni I in comparison with the stars having the massive brown dwarfs. The data suggest, as previously reported, that massive and low-mass brown dwarfs might present differences in period and eccentricity. We find evidence of a non-metallicity dependent mechanism for the formation of massive brown dwarfs. Our results agree with a scenario in which massive brown dwarfs are formed as stars. At high-metallicities, the core-accretion mechanism might become efficient in the formation of low-mass brown dwarfs while at lower metallicities low-mass brown dwarfs could form by gravitational instability in turbulent protostellar discs. | en_US |
dc.language.iso | eng | en_US |
dc.title | Searching for chemical signatures of brown dwarf formation | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201630120 | en_US |
dc.identifier.scopus | 2-s2.0-85020173510 | en_US |
dc.identifier.isi | 000404648300075 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/abs/2017/06/aa30120-16/aa30120-16.html | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 602 | en_US |
dc.relation.firstpage | A38 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | ESP | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | ASTRONOMY & ASTROPHYSICS | en_US |
dc.type.miur | 262 Articolo in rivista | en_US |
dc.identifier.adsbibcode | 2017A&A...602A..38M | en_US |
dc.relation.ercsector | ERC sectors::Physical Sciences and Engineering::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_6 Stars and stellar systems | 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.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Palermo | - |
crisitem.author.orcid | 0000-0002-2218-5689 | - |
crisitem.journal.journalissn | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
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jesusmp_aa30120-16.pdf | PDF editoriale | 773.55 kB | Adobe PDF | View/Open |
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