Computer Science – Numerical Analysis
Scientific paper
Feb 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979m%26p....20...15g&link_type=abstract
(Conference on Protostars and Planets, Tucson, Ariz., Jan. 3-7, 1978.) Moon and the Planets, vol. 20, Feb. 1979, p. 15-48.
Computer Science
Numerical Analysis
7
Cosmic Dust, Interstellar Matter, Protostars, Solar System, Stellar Evolution, Angular Momentum, Graphs (Charts), Mass Distribution, Numerical Analysis, Solar Rotation, Spin Dynamics, Star Clusters, Stellar Mass
Scientific paper
Prestellar interstellar dust is discussed in terms of the evolution of dust grains. Two populations of dust grains - large core-mantle grains and very small bare particles - are distinguished. It is suggested that the cores are approximately 0.05-micron silicate while the mantles consist of a size distribution of photoprocessed accreted thicknesses of C, N, O molecules and radicals with an outer layer of molecules (mostly CO) and other species accreted in the later stages of cloud contraction. Most of the mantles contain stored energy. The maximum mean size of the core-mantle particles is approximately 0.21 microns, while the as yet unidentified bare particles are assumed to have a mean size of approximately 0.005 microns and to be about 3000-4000 times as numerous as the core particles. Physical arguments are presented to explain the narrow size distribution of the two types of particles. A laboratory analog of photoprocessing of interstellar grains is considered.
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