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  1. OA@INAF
  2. PRODOTTI RICERCA INAF
  3. 1 CONTRIBUTI IN RIVISTE (Journal articles)
  4. 1.01 Articoli in rivista
Please use this identifier to cite or link to this item: http://hdl.handle.net/20.500.12386/31188
DC FieldValueLanguage
dc.contributor.authorAbia, C.en_US
dc.contributor.authorde Laverny, P.en_US
dc.contributor.authorCRISTALLO, Sergioen_US
dc.contributor.authorKordopatis, G.en_US
dc.contributor.authorStraniero, O.en_US
dc.date.accessioned2021-11-30T13:32:04Z-
dc.date.available2021-11-30T13:32:04Z-
dc.date.issued2020en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/20.500.12386/31188-
dc.description.abstractWe 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.isoengen_US
dc.titleProperties of carbon stars in the Solar neighbourhood based on Gaia DR2 astrometryen_US
dc.typeArticle-
dc.identifier.doi10.1051/0004-6361/201936831en_US
dc.identifier.scopus2-s2.0-85088046784en_US
dc.identifier.isiWOS:000508595600001en_US
dc.identifier.urlhttps://www.aanda.org/articles/aa/full_html/2020/01/aa36831-19/aa36831-19.htmlen_US
dc.identifier.urlhttp://arxiv.org/abs/1911.09413v1en_US
dc.relation.mediumSTAMPAen_US
dc.relation.volume633en_US
dc.relation.firstpageA135en_US
dc.type.refereeREF_1en_US
dc.description.numberofauthors5en_US
dc.description.internationalsìen_US
dc.contributor.countryITAen_US
dc.contributor.countryFRAen_US
dc.contributor.countryESPen_US
dc.relation.scientificsectorFIS/05 - ASTRONOMIA E ASTROFISICAen_US
dc.relation.journalASTRONOMY & ASTROPHYSICSen_US
dc.type.miur262 Articolo in rivista-
dc.identifier.adsbibcode2020A&A...633A.135Aen_US
dc.description.apcnoen_US
dc.description.oa1 – prodotto con file in versione Open Access (allegare il file al passo  5-Carica)en_US
item.openairetypeArticle-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_18cf-
item.languageiso639-1en-
item.cerifentitytypePublications-
item.fulltextWith Fulltext-
crisitem.journal.journalissn0004-6361-
crisitem.journal.anceE016240-
crisitem.author.deptO.A. Abruzzo-
crisitem.author.orcid0000-0001-9683-9406-
Appears in Collections:1.01 Articoli in rivista
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