Analytical electron microscopy of fine-grained phases in primitive interplanetary dust particles and carbonaceous chondrites

Details Analytical electron microscopy of fine-grained phases in primitive interplanetary dust particles and carbonaceous chondrites Analytical electron microscopy of fine-grained phases in primitive interplanetary dust particles and carbonaceous chondrites

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pggp.rept...87m&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986 p 87-89 (SEE N87-23341 16-91)

Physics

Geophysics

Carbonaceous Chondrites, Chemical Composition, Interplanetary Dust, Electron Microscopy, Mineralogy, Particle Size Distribution, Temperature Dependence

Scientific paper

In order to describe the total mineralogical diversity within primitive extraterrestrial materials, individual interplanetary dust particles (IDPs) collected from the stratosphere as part of the JSC Cosmic Dust Curatorial Program were analyzed using a variety of AEM techniques. Identification of over 250 individual grains within one chondritic porous (CP) IDP shows that most phases could be formed by low temperature processes and that heating of the IDP during atmospheric entry is minimal and less than 600 C. In a review of the mineralogy of IDPs, it was suggested that the occurrence of other silicates such as enstatite whiskers is consistent with the formation in an early turbulent period of the solar nebula. Experimental confirmation of fundamental chemical and physical processes in a stellar environment, such as vapor phase condensation, nucleation, and growth by annealing, is an important aspect of astrophysical models for the evolution of the Solar System. A detailed comparison of chondritic IDP and carbonaceous chondrite mineralogies shows significant differences between the types of silicate minerals as well as the predominant oxides.

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