Computer Science
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29..508n&link_type=abstract
Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 508-509
Computer Science
6
Forsterite, Gas-Solid Interfaces, Hydrogen, Magnesium Compounds, Silicon Compounds, Solar Corona, Vaporizing, Activation Energy, Evaporation, Mineralogy, Pressure Effects
Scientific paper
Forsterite is one of the most prominent minerals in the solar system, and its vaporization behavior should be studied in detail for the understanding of the Mg-Si and isotopic fractionation. Hashimoto and Wang et al. measured the evaporation rate of forsterite in vacuum, which is expected to be much smaller than that in the presence of H gas from the study of SiO2 vaporization in vacuum and H gas. Vaporization rate of forsterite was determined in a wide range of H gas pressure, and the results are reported with an application to vaporization processes in the solar nebula. The term 'vaporization' is used for transformation of solid to vapor in general, and 'evaporation' is used strictly for free evaporation typically realized in the Langmuir experiment. The results are applied to estimate the limit of residence time of forsterite dusts in the solar nebula. The time of total evaporation of a sphere of forsterite with radius of 0.1 microns to 1 cm was calculated. Within the plausible range of H pressure in the solar nebula, forsterite vaporizes very quickly. Even a grain with 1 mm radius completely vaporizes in a few days at 1700 C. If the activation energy for the reaction is similar to that of evaporation of forsterite determined by Hashimoto, the grain completely vaporizes in a month at 1600 C. Because the experiments were made in molecular flow of H gas that is continuously evacuated, the estimated vaporization time probably gives the lower limit.
Nagahara Hiroki
Ozawa Kazuhito
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