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Are extreme asympto...
Are extreme asymptotic giant branch stars post-common envelope binaries?
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- Dell'Agli, F. (author)
- INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy.
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- Marini, E. (author)
- INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy.;Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00100 Rome, Italy.
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- D'Antona, F. (author)
- INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy.
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- Ventura, P. (author)
- INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy.
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- Groenewegen, M. A. T. (author)
- Koninklijke Sterrenwacht Belgie, Ringlaan 3, Brussels, Belgium.,Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy.
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- Mattsson, Lars (author)
- Stockholms universitet,KTH,Nordic Institute for Theoretical Physics NORDITA,Nordiska institutet för teoretisk fysik (Nordita)
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- Kamath, D. (author)
- Macquarie Univ, Dept Phys & Astron, Sydney, NSW 2109, Australia.
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- Garcia-Hernandez, D. A. (author)
- Inst Astrofis Canarias IAC, E-38205 Tenerife, Spain.;Univ La Laguna ULL, Dept Astrofis, E-38206 Tenerife, Spain.
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- Tailo, M. (author)
- Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy.
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INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy INAF, Observ Rome, Via Frascati 33, I-00077 Monte Porzio Catone, RM, Italy.;Univ Roma Tre, Dipartimento Matemat & Fis, Via Vasca Navale 84, I-00100 Rome, Italy. (creator_code:org_t)
- 2021-01-22
- 2021
- English.
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In: Monthly notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966 .- 1745-3925 .- 1745-3933. ; 502:1, s. L35-L39
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https://academic.oup...
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https://urn.kb.se/re...
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https://doi.org/10.1...
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Abstract
Subject headings
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- Modelling dust formation in single stars evolving through the carbon-star stage of the asymptotic giant branch (AGB) reproduces well the mid-infrared colours and magnitudes of most of the C-rich sources in the Large Magellanic Cloud (LMC), apart from a small subset of extremely red objects (EROs). An analysis of the spectral energy distributions of EROs suggests the presence of large quantities of dust, which demand gas densities in the outflow significantly higher than expected from theoretical modelling. We propose that binary interaction mechanisms that involve common envelope (CE) evolution could be a possible explanation for these peculiar stars; the CE phase is favoured by the rapid growth of the stellar radius occurring after C/O overcomes unity. Our modelling of the dust provides results consistent with the observations for mass-loss rates (M) over dot similar to 5 x 10(-4) M-circle dot yr(-1), a lower limit to the rapid loss of the envelope experienced in the CE phase. We propose that EROs could possibly hide binaries with orbital periods of about days and are likely to be responsible for a large fraction of the dust production rate in galaxies.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
- NATURVETENSKAP -- Fysik (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences (hsv//eng)
Keyword
- stars: AGB and post-AGB
- binaries (including multiple): close
- stars: carbon
- stars: mass-loss
- dust
- extinction
- Magellanic Clouds
Publication and Content Type
- ref (subject category)
- art (subject category)
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