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http://hdl.handle.net/20.500.12386/31188
Titolo: | Properties of carbon stars in the Solar neighbourhood based on Gaia DR2 astrometry | Autori: | Abia, C. de Laverny, P. CRISTALLO, Sergio Kordopatis, G. Straniero, O. |
Data pubblicazione: | 2020 | Rivista: | ASTRONOMY & ASTROPHYSICS | Numero: | 633 | Da pagina:: | A135 | 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. | URI: | http://hdl.handle.net/20.500.12386/31188 | URL: | https://www.aanda.org/articles/aa/full_html/2020/01/aa36831-19/aa36831-19.html http://arxiv.org/abs/1911.09413v1 |
ISSN: | 0004-6361 | DOI: | 10.1051/0004-6361/201936831 | Bibcode ADS: | 2020A&A...633A.135A | Fulltext: | open |
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