Computer Science
Scientific paper
Jun 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984sciam.250..124g&link_type=abstract
Scientific American (ISSN 0036-8733), vol. 250, June 1984, p. 124-133, 135.
Computer Science
29
Cosmic Dust, Cosmochemistry, Interstellar Chemistry, Interstellar Matter, Comets, Infrared Absorption, Interstellar Extinction, Molecular Clouds, Radicals, Water, Cosmic Dust, Interstellar Dust, Structure, Evolution, Cores, Mantles, Features, Characteristics, Organic Compounds, Chemistry, Wavelengths, Formation, Grains, Photographs, Equipment, Spectra, Data, Infrared, Absorption, Radiation, Diagrams, Comets, Composition
Scientific paper
A mixture of water, methane, ammonia, and additional simple molecules are introduced into an experimental chamber, and the evolution of interstellar grains and the gaseous clouds in which they are found is consequently proposed. A grain begins in a diffuse cloud and already has a mantle of yellow stuff. The cloud becomes denser, and the grains accrete a layer of ices. Ultraviolet irradiation generates radicals in the grains' icy mantle, and subsequent collisions among the grains heat the mantle enough for radicals to recombine. The mantle may explode and repopulate the gaseous phase of the cloud. In the densest areas of the cloud, gravitational collapse of gas and dust effects star formation; the icy grain mantle is evaporated and the yellow stuff remains. Grains not included in the star formation return to the diffuse cloud environment. Consideration is also given to the extinction of starlight by interstellar grains, the spectrum of the Becklin-Neugebauer object, the infrared spectrum of the yellow stuff, and the spectrum of an infrared source designated W33.
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