Messung der Zugänglichkeit an Celluloseoberflächen mittels Infrarotspektroskopie

Anders, H. E.; Malsch, G.; Paul, Dipayan

doi:10.1002/actp.1989.010400616

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Fine-grained Dust and Chondmle Fe1

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1998

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“…The figure shows that 1 km behind the shock, a 10-pm particle and a 100-pm particle collide at -0.35 times the post-shock gas speed; whereas 1000 km behind the shock, a 1 -cm particle and a Total gas pessure during chondn.de formation. 'Molten chondrules are unstable and will evaporate under pressures of bar (the canonical protoplanetary nebula ambient pressure) in a gas of solar composition (2,38). The rate of evaporation is poorly known (18,39,40).…”

Section: Fine-grained Dust and Chondmle Fementioning

confidence: 99%

The Formation of Chondrules: Petrologic Tests of the Shock Wave Model

Connolly

Love

1998

Science

127

113

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Chondrules are millimeter-sized rounded igneous rocks within chondritic meteorites. Their textures and fractionated mineral chemistries suggest that they formed by repeated, localized, brief (minutes to hours) melting of cold aggregates of mineral dust in the protoplanetary nebula. Astrophysical models of chondrule formation have been unable to explain the petrologically diverse nature of chondrites. However, a nebular shock wave model for chondrule formation agrees with many of the observed petrologic and geochemical properties of chondrules and shows how particles within the nebula are sorted by size and how rims around chondrules are formed. It also explains the volatile-rich nature of chondrule rims and the chondrite matrix.

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Section: Fine-grained Dust and Chondmle Fementioning

confidence: 99%