Coagulation of grains in static and collapsing protostellar clouds

Details Coagulation of grains in static and collapsing protostellar clouds Coagulation of grains in static and collapsing protostellar clouds

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24.1499w&link_type=abstract

In Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z p 1499-1500 (SEE N94-20636 05-91

Mathematics

1

Coagulation, Grain Size, Gravitational Collapse, Interstellar Extinction, Interstellar Matter, Meteoritic Microstructures, Molecular Clouds, Particle Size Distribution, Aggregates, Magnetohydrodynamic Stability, Mathematical Models, Meteoritic Composition, Meteoroid Concentration, Spatial Distribution, Temporal Distribution, Turbulence Effects

Scientific paper

The wavelength dependence of extinction in the diffuse interstellar medium implies that it is produced by particles of dominant size of approximately 10-5 cm. There is some indication that in the cores of dense molecular clouds, sub-micron grains can coagulate to form larger particles; this process is probably driven by turbulence. The most primitive meteorites (carbonaceous chondrites) are composed of particles with a bimodal size distribution with peaks near 1 micron (matrix) and 1 mm (chondrules). Models for chondrule formation that involve processing of presolar material by chemical reactions or through an accretion shock during infall assume that aggregates of the requisite mass could form before or during collapse. The effectiveness of coagulation during collapse has been disputed; it appears to depend on specific assumptions. The first results of detailed numerical modeling of spatial and temporal variations of particle sizes in presolar clouds, both static and collapsing, is reported in this article.

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