Pulse heating of fragments from Orgueil (CI): Simulation of atmospheric entry heating of micrometeorites

Details Pulse heating of fragments from Orgueil (CI): Simulation of atmospheric entry heating of micrometeorites Pulse heating of fragments from Orgueil (CI): Simulation of atmospheric entry heating of micrometeorites

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994metic..29..470g&link_type=abstract

Meteoritics (ISSN 0026-1114), vol. 29, no. 4, p. 470

Mathematics

Logic

8

Atmospheric Entry, Micrometeoroids, Orgueil Meteorite, Pulse Heating, Thermal Simulation, Chemical Effects, Earth Atmosphere, Mineralogy, Temperature Effects, Thermal Degradation

Scientific paper

Most micrometeorites and interplanetary dust particles (IDPs) suffer severe heating on entering the Earth's atmosphere. Depending on their entry velocity, entry angle, size, and density, 100-micron-sized unmelted micrometeoroids are heated to temperatures ranging from 700 to 1300 C. We are studying the chemical and mineralogical changes in pulse-heated Orgueil samples in order to estimate the peak temperatures experienced by micrometeoroids during atmospheric entry. Possible effects include Zn depletion, loss of solar flare tracks, magnetite rim formation, He-4 release, and laihunite formation. Very few results on mineralogical and chemical changes during flash-heating experiments exist. For our experiments, Orgueil meteorite fragments approximately 100 microns in size were used. The fragments were heated in a furnace and immediately cooled in water. All experiments were carried out in air temperatures ranging from 700 to 1250 C for 10-60 s. Every fragment was analyzed by proton-induced X-ray emission (PIXE) for volatile elements before and after heating. Gallium seems not to be volatile under oxidizing conditions up to 1300 C. In our experiments we observe that losses of volatile elements are strongly dependent on temperature and time. Volatile element losses except for Ga are consistent with the results of Wulf (1990). IDPs heated on atmospheric entry show depletions of Zn and less-pronounced depletions of Ga and Ge. The order of volatile element losses of these IDPs is Zn greater than Ge greater than Ga. In our experiments these three elements are depleted to similar extents. This deviation may be explained by the difference in the host phases of volatile elements in CI meteorites and IDPs.

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