Grain growth by radiation pressure induced coagulation

Details Grain growth by radiation pressure induced coagulation Grain growth by radiation pressure induced coagulation

Aug 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..71....3s&link_type=abstract

Astrophysics and Space Science, vol. 71, no. 1, Aug. 1980, p. 3-24. Research supported by the Science Research Council.

Astronomy and Astrophysics

Astrophysics

8

Coagulation, Grains, Interstellar Matter, Nucleation, Particle Collisions, Radiation Pressure, Astrophysics, Dense Plasmas, Growth, Protostars, Stellar Evolution, Turbulence Effects

Scientific paper

A theoretical treatment is given of the growth of grains as a consequence of their mutual coagulation brought about by relative motions induced by radiation pressure. Analytical and numerical techniques are employed to tackle the relevant coagulation equation. The results are of particular astrophysical significance in the context of forming very small grains following a nucleation process, in the production of grains large enough to allow condensation of volatiles onto their surface, and in any situation where the supply of volatiles has been exhausted. It was found that in interstellar clouds, grains composed of iron, graphite and glassy carbon, being typical examples of three basic types of material, could grow to a size where condensation of the volatiles was possible. On the other hand, olivine, a typical silicate, could not. If a source of radiation existed at the center of the cloud, then growth could occur if the cloud was turbulent or if the density was high enough; otherwise the grains were driven out of the regions of interest at high velocity. In the latter case, with a high cloud density, re-radiation has to be taken into account.

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