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Constraints on chondrule agglomeration from fine-grained chondrule rimsFine-grained rims around chondrules, Ca,Al-rich inclusions, and other coarse-grained components occur in most types of unequilibrated chondrites, most prominently in carbonaceous chondrites of the CM group. Based on mineralogical and petrographic investigations, it was suggested that rim structures in unequilibrated ordinary chondrites could have formed in the solar nebula by accretion of dust on the surfaces of the chondrules. Dust mantles in CM chondrites seem to have formed by accretion of dust on the surfaces of chondrules and other components during their passage through dust-rich regions in the solar nebula. Concentric mantles with compositionally different layers prove the existence of various distinct dust reservoirs in the vicinity of the accreting parent body. Despite mineralogical and chemical differences, fine-grained rims from other chondrite groups principally show striking similarities to dust mantle textures in CM chondrite. This implies that the formation of dust mantles was a cosmically significant event like the chondrule formation itself. Dust mantles seem to have formed chronologically between chondrule-producing transient heating events and the agglomeration of chondritic parent bodies. For this reason the investigation of dust mantle structures may help to answer the question of how a dusty solar nebula was transformed into a planetary system.
Document ID
19950012900
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Metzler, K.
(Humboldt Univ. Berlin (German D.R.)., United States)
Bischoff, A.
(Muenster Univ. Germany)
Date Acquired
September 6, 2013
Publication Date
January 1, 1994
Publication Information
Publication: Lunar and Planetary Inst., Papers Presented to the Conference on Chondrules and the Protoplanetary Disk
Subject Category
Astrophysics
Accession Number
95N19315
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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