title: Are some chondrule rims formed by impact processes?  Observations and experiments.
abstract: Observations and experimental evidence are presented to support the hypothesis that high-speed impact into a parent body regolith can best explain certain textures and compositions observed for rims on some chondrules.  A study of 19 interclastic rimmed chondrules in the Weston (H 3/4) ordinary chondrite shows that two main rim types are present on porphyritic olivine-pyroxene (POP) and porphyritic pyroxene (PP) chondrules:  granular and opaque rims.  Granular rims are composed of welded, fine-grained host chondrule fragments.  Bulk compositions of granular rims vary among chondrules, but each rim is compositionally dependent on that of the host chondrule.  Opaque rims contain mineral and glass compositions distinctly different from those of the host, partially reacted chondrule mantle components, and some matrix grains.  Opaque rims are greatly enriched in FeO (up to 63 wt%).  The original chondrule pyroxene compositional zonation patterns and euhedral grain outlines are discontinuous at the chondrule/rim interface.  Opaque rims are dominated by fayalitic olivine (Fa92-56), with high Al2O3 content (0.78-3.15%), which makes them distinctly different from primary olivine, but similar to Fe-olivine in chondrule rims of other meteorites.  Thin zones of chondrule minerals adjacent to the present rims are intermediate in FeO content between the Mg-rich interior and the Fe-rich rim, which indicates a reaction relationship.  Regardless of conclusions drawn regarding other types of rims, granular and opaque rim characteristics appear to be inconsistent with nebular condensation, in that host and matrix fragments are included within the rim.  We have initiated a series of experiments, using the Ames two-stage light gas gun, to investigate the hypothesis that the Weston chondrule rims are the result of thermal and mechanical alteration upon impact into a low-density medium.  Clusters of approximately 200-micron-sized silicate particles were fired into aerogel (density = 0.1 g cm-3) at velocities of 5.6, 4.7, and 2.2 km sec-1.  Recovered grains show characteristics that range from fragmented projectile grains mixed with melted aerogel that nearly rim the grains to grains that have melted aerogel clumps mixed with partially melted projectile.  These experimental results demonstrate that rim-like thermal and mechanical alteration of projectiles can result from a high-velocity encounter with a low-density target.  Therefore, experiments using appropriately chosen projectile and target materials can provide a test of the hypothesis that chondrule rims common to Weston and possibly other ordinary chondrites were formed by such a process.
authors.affiliation: NASA Ames Research Center, Moffett Field, California 94035, USA.
authors.forename: T E
authors.initials: TE
authors.lastname: Bunch
authors.forename: P
authors.initials: P
authors.lastname: Schultz
authors.forename: P
authors.initials: P
authors.lastname: Cassen
authors.forename: D
authors.initials: D
authors.lastname: Brownlee
authors.forename: M
authors.initials: M
authors.lastname: Podolak
authors.forename: J
authors.initials: J
authors.lastname: Lissauer
authors.forename: R
authors.initials: R
authors.lastname: Reynolds
authors.forename: S
authors.initials: S
authors.lastname: Chang
mesh_terms: D055580:Astronomical Phenomena; D001256:Astronomy; D003460:Crystallization; D055593:Geological Phenomena; D005844:Geology; D005898:Glass; D058085:Iron Compounds / Q000737:chemistry*; D017616:Magnesium Compounds / Q000737:chemistry*; D008903:Minerals / Q000737:chemistry*; D018543:Minor Planets; D008962:Models, Theoretical; D017640:Silicates / Q000737:chemistry*; D016082:Solar System
chemical_list: D058085:Iron Compounds; D017616:Magnesium Compounds; D008903:Minerals; D017640:Silicates; C092478:pyroxene; C034475:olivine