Evolution of density in solar system ices

Details Evolution of density in solar system ices Evolution of density in solar system ices

Jun 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984em%26p...30..281s&link_type=abstract

Earth, Moon, and Planets (ISSN 0167-9295), vol. 30, June 1984, p. 281-288.

Other

14

Ice, Interplanetary Medium, Solar System, Carbon Dioxide, Densification, Icy Satellites, Porosity, Temperature Gradients, Water

Scientific paper

Pores present in ices in the solar system do not remain unchanged. In isothermal conditions they shrink while in a thermal gradient they migrate towards the higher temperature and escape so that the ice densifies. This motion has been investigated for pure H2O- and CO2-ices in a very simple one-dimensional model assuming uniform thermal conductivity and temperature gradient. The results indicate that the densification of H2O-ice is so slow that it could be significant only for icy satellites having an internal heat source. On the other hand, CO2-ice densifies orders of magnitude faster and the effect should be important for the CO2 component of cometary nuclei. No effect is expected for icy planetary rings.

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