Do evolved stars in the LMC show dual dust chemistry?

Bibcode
2019MNRAS.488L..85M
DOI
10.1093/mnrasl/slz105
Marini, E.; Dell'Agli, F.; García-Hernández, D. A.; Groenewegen, M. A. T.; Puccetti, S.; Ventura, P.; Villaver, E.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society: Letters, Volume 488, Issue 1, p.L85-L89

Advertised on:
9
2019
Number of authors
7
IAC number of authors
2
Citations
4
Refereed citations
4
Description
We study a group of evolved M-stars in the Large Magellanic Cloud, characterized by a peculiar spectral energy distribution. While the 9.7 μm feature arises from silicate particles, the whole infrared data seem to suggest the presence of an additional featureless dust species. We propose that the circumstellar envelopes of these sources are characterized by a dual dust chemistry, with an internal region, harbouring carbonaceous particles, and an external zone, populated by silicate, iron, and alumina dust grains. Based on the comparison with results from stellar modelling that describe the dust formation process, we deduce that these stars descend from low-mass (M < 2 M⊙) objects, formed 1-4 Gyr ago, currently evolving either in the post-AGB phase or through an after-pulse phase, when the shell CNO nuclear activity is temporarily extinguished. Possible observations able to confirm or disregard the present hypothesis are discussed.
Related projects
Project Image
Nucleosynthesis and molecular processes in the late stages of Stellar Evolution
Low- to intermediate-mass (M < 8 solar masses, Ms) stars represent the majority of stars in the Cosmos. They finish their lives on the Asymptotic Giant Branch (AGB) - just before they form planetary nebulae (PNe) - where they experience complex nucleosynthetic and molecular processes. AGB stars are important contributors to the enrichment of the
Domingo Aníbal
García Hernández
In progress
Type
Refereed
Exoplanetary Systems & Solar System (SEYSS)
Stellar & Interstellar Physics (FEEI)
The Milky Way and the Local Group (MWLG)
Magellanic Clouds

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