We present dust yields for asymptotic giant branch ( AGB ) and super–asymptotic giant branch ( SAGB ) stars of solar metallicity .
Stars with initial mass 1.5 ~ { } M _ { \odot } \leq M _ { ini } \leq 3 ~ { } M _ { \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 the mass of the star ; the carbon grains with the largest size ( a _ { C } \sim 0.2 \mu m ) are produced by AGB stars with M _ { ini } = 2.5 - 3 ~ { } M _ { \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 _ { 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 _ { ini } > 3 ~ { } M _ { \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 _ { ol } < 0.15 \mu m and a _ { Al _ { 2 } O _ { 3 } } \sim 0.07 \mu m , respectively .
The mass of silicates produced spans the interval 3.4 \times 10 ^ { -3 } ~ { } M _ { \odot } \leq M _ { dust } \leq 1.1 \times 10 ^ { -2 } ~ { } M _ { \odot } and increases with the initial mass of the star .