AGB and SAGB stars: modelling dust production at solar metallicity

Abstract

We present dust yields for asymptotic giant branch (AGB) and super--asymptotic giant branch (SAGB) stars of solar metallicity. Stars with initial mass $1.5M_{\odot }\le M_{\mathrm{ini}}\le 3M_{\odot }$ reach the carbon star stage during the AGB phase and produce mainly solid carbon and SiC. The size and the amount of the carbon particles formed follows a positive trend with themass of the star; the carbon grains with the largest size ($a_{\mathrm{C}}\sim 0.2\mu$m) are produced by AGB stars with $M_{\mathrm{ini}}=2.5-3M_{\odot }$, as these stars are those achieving the largest enrichment of carbon in the surface regions. The size of SiC grains, being sensitive to the surface silicon abundance, keeps around $a_{\mathrm{SiC}}\sim 0.1\mu$m. The mass of carbonaceous dust formed is in the range $10^{-4}-5\times 10^{-3}{M}_{\odot }$, whereas the amount of SiC produced is $2\times 10^{-4}-10^{-3}{M}_{\odot }$. Massive AGB/SAGB stars with $M_{\mathrm{ini}}>3M_{\odot }$ experience HBB, that inhibits formation of carbon stars. The most relevant dust species formed in these stars are silicates and alumina dust, with grain sizes in the range $0.1\mu m<a_{\mathrm{ol}}<0.15\mu$m and $a_{\mathrm{A}{\mathrm{l}}_2{\mathrm{O}}_3}\sim 0.07\mu$m, respectively. The mass of silicates produced spans the interval $3.4\times 10^{-3}{M}_{\odot }\le M_{\mathrm{dust}}\le 1.1\times 10^{-2}{M}_{\odot }$ and increases with the initial mass of the star.

Accepted for publication in MNRAS

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