Formation conditions of pyroxene-olivine and magnesian olivine chondrules

Details Formation conditions of pyroxene-olivine and magnesian olivine chondrules Formation conditions of pyroxene-olivine and magnesian olivine chondrules

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990gecoa..54.3475r&link_type=abstract

Geochimica et Cosmochimica Acta (ISSN 0016-7037), vol. 54, Dec. 1990, p. 3475-3490.

Computer Science

36

Chondrule, Meteoritic Composition, Meteoritic Microstructures, Olivine, Pyroxenes, Transient Heating, Granular Materials, Solar Corona, Solar System

Scientific paper

Dynamic crystallization experiments performed on a Type I and an intermediate Type II/III composition demonstrate chondrule texture is controlled by the abundance of heterogeneous nuclei. This factor is controlled by the maximum initial temperature relative to the olivine disappearance temperature for the given heating time. Glassy and excentroradial textures form from superheated melts with no nuclei, and barred textures form with initial temperatures near the olivine disappearance temperature. Porphyritic and granular textures form with initial temperatures below the liquidus with abundant nuclei. Comparison of zoning characteristics of experimental olivines with those in natural porphyritic olivine chondrules indicates cooling rates of 100 to 1000 C/h, whereas olivine morphology indicates barred olivines cooled at rates of 250 to 1000 C/h. Texture/composition relationships suggest chondrules experienced initial temperatures below 1750 C. These observations are consistent with the idea that chondrules formed by transient heating in dust-rich regions (i.e., in the midplane) of the solar nebula.

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