Asymptotic giant branch and super-asymptotic giant branch stars: modelling dust production at solar metallicity

作者：Dell' Agli F; Garcia Hernandez D A; Schneider R; Ventura P; La Franca F; Valiante R; Marini E; Di Criscienzo M

来源：Monthly Notices of the Royal Astronomical Society, 2017, 467(4): 4431-4440.

DOI：10.1093/mnras/stx387

• stars: abundances
• stars: AGB and post-AGB
• stars: carbon
• dust
• extinction

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(circle dot)= M-ini = 3M 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 the mass of the star; the carbon grains with the largest size (a(C) similar to 0.2 mu m) are produced by AGB stars with M-ini = 2.5-3M, as these stars are those achieving the greatest enrichment of carbon in the surface regions. The size of SiC grains, being sensitive to the surface silicon abundance, remains at about a(SiC) similar to 0.1 ae m. The mass of carbonaceous dust formed is in the range 10-45x10- 3M, whereas the mass of SiC produced is 2x10-4-10-3M. Massive AGB/SAGB stars with M-ini > 3M experience hot bottom burning, which inhibits the formation of carbon stars. The most relevant dust species formed in these stars are silicate and alumina dust, with grain sizes in the range 0.1 < a(ol) < 0.15 mu m and a(Al2O3) similar to 0.07 ae m, respectively. The mass of silicates produced spans the interval 3.4 x 10-3M = Mdust = 1.1 x 10-2M and increases with the initial mass of the star.

• 出版日期2017-6