Computer Science
Scientific paper
Sep 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987esasp.278..509r&link_type=abstract
In ESA, Proceedings of the International Symposium on the Diversity and Similarity of Comets p 509-513 (SEE N88-21884 14-91)
Computer Science
1
Comet Nuclei, Comets, Evolution (Development), Ice, Radiation Chemistry, Temperature Effects, Radiation Effects, Solar Wind, Systems Stability
Scientific paper
Comet evolution, particularly temperature effects, is discussed. The temperature of the surface of a young periodic comet rises from values much below 100 K to those beyond 200 K when reaching the inner solar system. The actual temperature depends on the orbit, in particular on the nearest distance to the Sun, and the age of the comet. Thermal effects such as phase transformations, the mobility of radiolytic radicals, destruction of clathrates or related water-volatile adducts, increase of gas pressure of volatiles, etc., may combine in a synergic way to explosive processes when crossing the temperature region between 100 and 170 K. This may explain the energetic dust jets observed on P/Halley. The radiation stability of organic compounds depends on the dose, the concentration of radicals formed, their mobility and reactivity. The synergic temperature effects may lead to an oxidation and destruction of organic monomeric compounds. Photolytic, radiolytic, and hot atom reactions of the solar radiation (photons and solar wind or flares) may induce the formation of thin crusts of organic polymers and refractories.
Nebeling B.
Roessler Kurt
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