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Formation and Evolution of Minerals in Accretion Disks and Stellar Outflows

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Astromineralogy

Part of the book series: Lecture Notes in Physics ((LNP,volume 815))

Abstract

The contribution discusses dust formation and dust processing in oxygen-rich stellar outflows under non-explosive conditions, and in circumstellar discs. The main topics are calculation of solid-gas chemical equilibria, the basic concepts for calculating dust growth under non-equilibrium conditions, dust processing by annealing and solid diffusion, a discussion of non-equilibrium dust formation in stellar winds, and in particular a discussion of the composition and evolution of the mineral mixture in protoplanetary accretion discs. An overview is given over the data on dust growth, annealing, and on solid diffusion for astrophysically relevant materials available so far from laboratory experiments.

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Notes

  1. 1.

    If necessary, other phases than gaseous ones are indicated by “s” for solids or “l” for liquid. In the present contribution we indicate this by adding a corresponding label in brackets after the chemical formula. E.g., the reaction corresponding to the sublimation of solid iron is written as follows: \(\mathrm{Fe(s)} \to \mathrm{Fe}\). Here Fe(s) denotes solid iron and Fe iron atoms in the gas phase

  2. 2.

    For instance, for \(\mathrm{MgSiO}_3\) the least abundant of the elements Mg, Si, and O in the cosmic element mixture is Mg. Then it would be appropriate to chose Mg as the reference element for defining a degree of condensation. However, because of a similar abundance of Mg and Si, an equally appropriate choice for the reference element would be Si. Generally the choice of a reference element for defining condensation degrees is to some extent arbitrary and one can chose that one which is the most convenient for the problem under consideration.

  3. 3.

    In case of element mixture No. 4 of Table 1 one has to use He as reference element for definition of abundances ε. The modifications required to all equations in that case are obvious.

  4. 4.

    For example: If j refers to \(\mathrm{Al}_2\mathrm{O}_3\) (corundum) and we define the degree of condensation f for corundum with respect to Al, and if k refers to oxygen, then one has in the contribution from corundum to the l.h.s of the equation for oxygen \(\nu_{j,k}=3/2\), since in the chemical formula there is 1.5 oxygen atom per aluminium atom. In the contribution to the equation for Al one has \(\nu_{j,k}=1\) because Al is the reference element for corundum.

  5. 5.

    also available at: http://webbook.nist.gov/chemistry/form-ser.html

  6. 6.

    The existence of chondrules in meteoritic material shows, however, that by local, not yet understood processes, some part of the disk matter was flash-heated to temperatures above the melting point.

  7. 7.

    Rotation of dust aggregates is neglected.

  8. 8.

    In Gail [99] the factor h was missing.

  9. 9.

    Dust temperatures may also be high in high layers of the disk photosphere where the dust is irradiated by the proto-star, but this region contains a negligible fraction of the total surface density \(\varSigma(r)\).

  10. 10.

    \(\mathrm{H}_2\mathrm{O}\) in any case is so abundant that abundance variations with varying degree of condensation of the silicates can be neglected.

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Acknowledgement

This work has been performed as part of the projects of the special research programmes SFB 359“Reactive flows, diffusion and transport” and SFB 439 “Galaxies in the Young Universe” and the Forschergruppe 759 “The formation of planets. The critical first growth phase” which are supported by the Deutsche Forschungsgemeinschaft (DFG).

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  1. Institute for Theoretical Astrophysics, Center for Astronomy, University of Heidelberg, Albert-Überle-Str. 2, 69120, Heidelberg, Germany

    H.-P. Gail

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    Thomas Henning

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Gail, HP. (2010). Formation and Evolution of Minerals in Accretion Disks and Stellar Outflows. In: Henning, T. (eds) Astromineralogy. Lecture Notes in Physics, vol 815. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-13259-9_2

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