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http://hdl.handle.net/20.500.12386/31188
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Abia, C. | en_US |
dc.contributor.author | de Laverny, P. | en_US |
dc.contributor.author | CRISTALLO, Sergio | en_US |
dc.contributor.author | Kordopatis, G. | en_US |
dc.contributor.author | Straniero, O. | en_US |
dc.date.accessioned | 2021-11-30T13:32:04Z | - |
dc.date.available | 2021-11-30T13:32:04Z | - |
dc.date.issued | 2020 | en_US |
dc.identifier.issn | 0004-6361 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/31188 | - |
dc.description.abstract | We find that the combined LF of N- and SC-type stars are consistent with a Gaussian distribution peaking at M_bol~ -5.2 mag. The resulting LF however shows two tails at lower and higher luminosities more extended than those previously found, indicating that AGB carbon stars with Solar metallicity may reach M_bol~-6.0 mag. We find that J-type stars are about half a magnitude fainter on average than N- and SC-type stars, while R-hot stars are half a magnitude brighter than previously found. The Galactic spatial distribution and velocity components of the N-, SC- and J-type stars are very similar, while about 30 % of the R-hot stars in the sample are located at distances larger than ~ 500 pc from the Galactic Plane, and show a significant drift with respect to the local standard of rest. The LF derived for N- and SC-type in the Solar neighbourhood fully agrees with the expected luminosity of stars of 1.5-3 M_o on the AGB. On a theoretical basis, the existence of an extended low luminosity tail would require a contribution of extrinsic low mass carbon stars, while the high luminosity one would imply that stars with mass up to ~5 Mo may become carbon star on the AGB. J-type stars not only differ significantly in their chemical composition with respect to the N- and SC-types but also in their LF, which reinforces the idea that these carbon stars belong to a dvifferent type whose origin is still unknown. The derived luminosities of R-hot stars make these stars unlikely to be in the red-clump as previously claimed. On the other hand, the derived spatial distribution and kinematic properties, together with their metallicity, indicate that most of the N-, SC- and J-type stars belong to the thin disc population, while a significant fraction of R-hot stars show characteristics compatible with the thick disc. | en_US |
dc.language.iso | eng | en_US |
dc.title | Properties of carbon stars in the Solar neighbourhood based on Gaia DR2 astrometry | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1051/0004-6361/201936831 | en_US |
dc.identifier.scopus | 2-s2.0-85088046784 | en_US |
dc.identifier.isi | WOS:000508595600001 | en_US |
dc.identifier.url | https://www.aanda.org/articles/aa/full_html/2020/01/aa36831-19/aa36831-19.html | en_US |
dc.identifier.url | http://arxiv.org/abs/1911.09413v1 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 633 | en_US |
dc.relation.firstpage | A135 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 5 | en_US |
dc.description.international | sì | en_US |
dc.contributor.country | ITA | en_US |
dc.contributor.country | FRA | 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 | - |
dc.identifier.adsbibcode | 2020A&A...633A.135A | 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 | 0004-6361 | - |
crisitem.journal.ance | E016240 | - |
crisitem.author.dept | O.A. Abruzzo | - |
crisitem.author.orcid | 0000-0001-9683-9406 | - |
È visualizzato nelle collezioni: | 1.01 Articoli in rivista |
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Abia_2020_A&A_633_135.pdf | Pdf editoriale | 1.02 MB | Adobe PDF | Visualizza/apri |
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