New calculations of interstellar dust (ID) contraction in a non-isothermal regime

Details New calculations of interstellar dust (ID) contraction in a non-isothermal regime New calculations of interstellar dust (ID) contraction in a non-isothermal regime

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ap%26ss.198..237e&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 198, no. 2, p. 237-251.

Astronomy and Astrophysics

Astrophysics

1

Cosmic Dust, Interstellar Gas, Interstellar Matter, Opacity, Electron Scattering, Hydrodynamic Equations, Mie Scattering, Poisson Equation, Protostars, Rayleigh Scattering, Star Formation

Scientific paper

We have calculated the opacity as resulting from different interstellar grain models, molecules, atoms, and ions. The resulting opacities have been applied to a numerical code used to follow the thermal evolution of a contracting cloud in one dimension. Exact analytical and computational developments of both Mie theory for isolated grains and Guettler's formulae for composite grain models have been used to calculate the extinction coefficients. We have studied two models of composite grain and three models of isolated grain. The opacity of interstellar grains has been calculated in the temperature range 10-1500 K. The molecular opacity is split into continuous and line opacities. The different sources of continuous opacity have been studied. The line opacity has also been included. The atomic opacities are also considered. The hydrodynamical equations are solved explicitly but the energy and Poisson equations are solved implicitly. It has been found that the thermal evolution during contraction of protostellar clouds is sensitive to both the assumed grain models and the considered chemical composition. A cloud of an initial temperature of 10 K collapsed to a stage in which the temperature increased to 91,000 K and the density reached to 0.16g/cu cm.

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