Grain coagulation in contracting protostellar clouds

Details Grain coagulation in contracting protostellar clouds Grain coagulation in contracting protostellar clouds

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251..587r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 2, Nov. 1991, p. 587-596. Research supported by FAPESP, FINEP, and CN

Astronomy and Astrophysics

Astrophysics

10

Gravitational Collapse, Interstellar Matter, Molecular Clouds, Protostars, Star Formation, Abundance, Particle Size Distribution, Turbulent Flow

Scientific paper

A numerical assessment of the processes capable of affecting the dust spectrum in dense molecular clouds is presented. The size spectrum is discretized and the time evolution of the spectral bins is computed, under the assumption of homogeneous and isothermal contraction. The influence of several assumed parameters, particularly the turbulence, is examined. The calculations are carried out up to a hydrogen density of 10 exp -11 g/cu cm, where the assumption regarding the isothermal behavior ceases to hold. The final spectrum departs considerably from the initial power law model. The average grain radius increases significantly due to vapor condensation during the first stages of contraction, and due to coagulation for densities higher than 10 exp -16 g/cu cm. The coagulation rate follows the turbulence parameter closely.

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