scholarly journals 9. Unusual Primitive Meteorites: Chondritic Inclusions from Group IAB Iron Meteorites

1977 ◽  
Vol 39 ◽  
pp. 397-402
Author(s):  
R. W. Bild
Keyword(s):  
Solar Nebula ◽  
Iron Meteorites ◽  
Silicate Inclusions ◽  
Additional Formation

Several meteorite types, distinct from the large chondrite groups (H, L, LL, E and carbonaceous), are known to also have chondritic compositions. These meteorites preserve information on conditions at additional formation locations in the early solar nebula. Silicate inclusions from group IAB iron meteorites are one such type. Evidence for their chondritic nature is given and their formation discussed.

scholarly journals The Relationship of Meteoritic Parent Body Thermal Histories and Electromagnetic Heating by a Pre-Main Sequence T Tauri Sun

1971 ◽  
Vol 12 ◽  
pp. 239-245 ◽  
Author(s):  
C.P. Sonett
Keyword(s):  
Main Sequence ◽  
Solar Nebula ◽  
Parent Body ◽  
Convincing Evidence ◽  
Iron Meteorites ◽  
T Tauri ◽  
Diffusion Studies ◽  
Thermal Histories ◽  
Relationship Of ◽  
The Relationship

Convincing evidence exists that meteoritic matter was reheated shortly after the initial condensation of the solar nebula for those meteorites thought to be derived from parent bodies. This evidence takes the form of cooling rates carefully determined from diffusion studies of the migration rate of Ni across kamacite-taenite boundaries in iron meteorites (Fish, Goles, and Anders, 1960; Goldstein and Ogilvie, 1965; Goldstein and Short, 1967; Wood, 1964). The notion that the irons condensed directly from the solar nebula requires that these measurements and the existence of large Widmanstätten figures be explained as a condensation event. This seems rather unlikely and, in any event, requires a far more complex explanation than heating and melting in a parent body.

scholarly journals 1. High-Temperature Condensates in Carbonaceous Chondrites

1977 ◽  
Vol 39 ◽  
pp. 507-516
Author(s):  
L. Grossman
Keyword(s):  
High Temperature ◽  
Trace Element ◽  
Solar Nebula ◽  
Trace Element Content ◽  
Group Iv ◽  
Carbonaceous Chondrites ◽  
Equilibrium Thermodynamic ◽  
Iron Meteorites ◽  
Solar Composition ◽  
Different Types

Equilibrium thermodynamic calculations of the sequence of condensation of minerals from a cooling gas of solar composition play an important role in explaining the mineralogy and trace element content of different types of inclusions in carbonaceous chondrites. Group IV B iron meteorites and enstatite chondrites may also be direct condensates from the solar nebula. Condensation theory provides a framework within which chemical fractionations between different classes of chondrites may be understood.

87Rb-87Sr ages of silicate inclusions in iron meteorites

1967 ◽  
Vol 2 (5) ◽  
pp. 397-408 ◽  
Author(s):  
D.S. Burnett ◽  
G.J. Wasserburg
Keyword(s):  
Iron Meteorites ◽  
Silicate Inclusions

Uranium in the silicate inclusions of stony-iron and iron meteorites

1982 ◽  
Vol 46 (5) ◽  
pp. 749-754 ◽  
Author(s):  
Ghislaine Crozaz ◽  
Scott F. Sibley ◽  
Douglas R. Tasker
Keyword(s):  
Iron Meteorites ◽  
Silicate Inclusions

Ages of Silicate Inclusions in Iron Meteorites

1968 ◽  
pp. 399-409
Author(s):  
D.S. BURNETT ◽  
G.J. WASSERBURG ◽  
D.D. BOGARD ◽  
P. EBERHARDT
Keyword(s):  
Iron Meteorites ◽  
Silicate Inclusions

scholarly journals 1. The Origin of Iron Meteorites

1977 ◽  
Vol 39 ◽  
pp. 405-413
Author(s):  
W. R. Kelly ◽  
E. R. Rambaldi ◽  
J. W. Larimer
Keyword(s):  
Melting Process ◽  
Iron Meteorites ◽  
Forming Process ◽  
Silicate Inclusions ◽  
Partial Melting Process ◽  
Group Iva ◽  
History Of ◽  
Advanced Stages ◽  
Flow Group ◽  
Cosmic History

The chemistry of iron meteorites is compared to predictions of the chemical fractionations that develop during the cosmic history of the metal phase, from condensation and accretion through melting, segregation and freezing. Of the 12 resolved iron meteorite groups, 3 appear to have evolved in bodies which accreted at T > 1000° K. In several cases, the core-forming process seems to have ceased prematurely, just as the metal began to melt and flow (group IAB with its silicate inclusions) or after the metal aggregated into pods but before it sank to form a core (group IVA, with groups IIAB and IIIAB being in more advanced stages). The Shaw chondrite contains residual metal from a partial melting process, as required to complement the fractional melts which refroze prematurely in the case of group IAB meteorites.

Xe and Kr analyses of silicate inclusions from iron meteorites

1971 ◽  
Vol 35 (12) ◽  
pp. 1231-1254 ◽  
Author(s):  
D.D Bogard ◽  
J.C Huneke ◽  
D.S Burnett ◽  
G.J Wasserburg
Keyword(s):  
Iron Meteorites ◽  
Silicate Inclusions
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