Physics and Chemistry of Circumstellar Dust Shells by Gail H.-P., Sedlmayr E.

By Gail H.-P., Sedlmayr E.

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The lines of constant mass-loss rate, according to a Reimers approximation (dotted lines), are labeled by ˙ in units of M yr−1 . 5 (from left to right). The thick rates from 10−9 to 10−4 M yr−1 in steps of log M line with circles indicates the transition line where the mass loss due to pulsation exceeds the mass-loss as given by a Reimers approximation. The thick line with filled circles indicates the transition line to optically very thick dust shells. ) at the same time the effective temperature is less than about 3,100 K the stars become Mira variables with pulsation periods P 300 d.

On the AGB, the low- and intermediate-mass stars all evolve through a stage where for several 29 30 Evolutionary Status of Dust-Enshrouded Objects 105 years or even for a few million years, they are enshrouded by optically thick circumstellar dust shells. 2. Massive stars with initial masses exceeding approximately Mec = 11 M finally explode as core-collapse supernovas. From the group of massive stars only those with initial masses less than approximately 40 M reach the RGB evolutionary stage and develop during a short phase very thick dust shells.

9). This allows a direct study of stellar nuclear burning processes and their by-products by laboratory investigations and a comparison of the results of laboratory investigations with model calculation predictions for different stellar types. Of particular interest in our context is the potential to identify the parent stars of individual dust grains in this way. By measuring certain isotopic abundances, one can sort out from an ensemble of presolar dust grains those which condensed in the circumstellar shells of giant stars.

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