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Prinz, Martin

Publications and source records attributed to Prinz, Martin.

11 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1994

The evolution of enstatite and chondrules in unequilibrated enstatite chondrites: Evidence from iron-rich pyroxene

FeO-rich (Fs(sub 6)-34) pyroxene lacking cathodoluminescence (CL), hereafter black pyroxene, is a major constituent of some of the chondrules and fragments in unequilibrated (type 3) enstatite chondrites (UECs). It contains structurally oriented zones of Cr-, Mn-, V-rich, FeO-poor enstatite with red CL, associated with mm-sized blebs of low-Ni, Fe-metal and, in some cases, silica. These occurrences represent clear evidence of pyroxene reduction. The black pyroxene is nearly always rimmed by minor element (Cr, Mn, V)-poor enstatite having a blue CL. More commonly, red and blue enstatites, unassociated with black pyroxene, occur as larger grains in chondrules and fragments, and these constitute the major silicate phases in UECs. The rare earth element (REE) abundance patterns of the black pyroxene are LREE-depleted. The blue enstatite rims, however, have a near-flat to LREE-enriched pattern, approx. 0.5-4x chondritic. The petrologic and trace element data indicate that the black pyroxene is from an earlier generation of chondrules that formed in a nebular region that was more oxidizing than that of the enstatite chondrites. Following solidification, these chondrules experienced a more reducing nebular environment and underwent reduction. Some, perhaps most, of the red enstatite that is common throughout the UECs may be the product of solid-state reduction of black pyroxene. The blue enstatite rims grew onto the surfaces of the black pyroxene and red enstatite as a result of condensation from a nebular gas. The evolutionary history of some of the enstatite and chondrules in enstatite chondrites can be expressed in a four-stage model that includes: Stage 1. Formation of chondrules in an oxidizing nebular environment. Stage 2. Solid-state reduction of the more oxidized chondrules and fragments to red enstatite in a more reducing nebular environment. Stage 3. Formation of blue enstatite rims on the black pyroxene as well as on the red enstatite. Stage 4. Reprocessing, by various degrees of melting, of many of the earlier-formed materials.

Weisberg, Michael K.↗
NASA NTRS1993

Carbonate compositions in CM and CI chondrites, and implications for aqueous alteration

Carbonate minerals in fourteen CM chondrites and two CI chondrites have been analyzed by electron microprobe to provide a better understanding of the aqueous processes that affected carbonaceous chondrite parent bodies. Calcites in CM chondrites and dolomites and magnesites in CI chondrites display the compositions expected of stable phases formed at low temperatures. Dolomites in CM chondrites, identified here for the first time in five members of the group, have small amounts of excess Ca which may reflect metastable growth. The distribution of Fe between dolomite and coexisting serpentine differs in the two chondrite groups. If the distributions reflect an approach to chemical equilibrium, then the difference implies higher alteration temperatures for the CI group than the CM group in agreement with the results of previously published oxygen isotope thermometry and mineral solubility modeling of the alteration process. Dolomite Fe contents are relatively uniform in the two chondrite groups. Dolomite Mn contents, by contrast, vary widely. The variations may reflect transport-controlled coprecipitation of Mn resulting from a heterogeneous distribution of the element in the anhydrous precursor material. If this interpretation is correct, then the altering fluids were essentially immobile white hydration reactions proceeded on the meteorite parent bodies. The near closed-system character of the alteration process, long known from bulk chemical analyses of the meteorites, is a direct consequence of the limited mobility of dissolved species.

Johnson, Craig A.↗
NASA NTRS1993

The CR (Renazzo-type) carbonaceous chondrite group and its implications

A petrologic, geochemical, and oxygen isotropic study of the CR chondrites including Renazzo, Al Rais, El Djouf 001 and the paired Acfer meteorites, EET87770 and the paired samples, MAC87320, Y790112, Y793495, and Y791498 is presented. It is concluded that the CR group is characterized by abundant large multilayered, Fe, Ni metal-rich, type I chondrules; abundant matrix and dark inclusions; unique assemblages of serpentine and chlorite-rich phyllosilicates and Ca-carbonates; Ca-carbonate rims on chondrules; abundant Fe, Ni metal with a positive Ni vs. Co trend and a solar Ni:Co ratio; and amoeboid olivine aggregates with Mn-rich and Mn-poor forsterite.

Weisberg, Michael K.↗
NASA NTRS1993

Trace element distributions in primitive achondrites

The primitive achondrites have approximately chondritic bulk chemical composition but achondritic textures. Clayton et al. show that nine of these meteorites, the acapulcoites and the lodranites, have similar oxygen isotopic compositions. The acapulcoites appear to be highly metamorphosed, but undifferentiated meteorites of chondritic composition; whereas, the lodranites appear to have lost a feldspathic partial melt. In order to learn more about metamorphic processes and partial melt removal, we have measured the trace element compositions of constituent phases of a number of primitive achondrites by ion microprobe. We have analyzed two acapulcoites, Acapulco and ALH81261 (paired with ALH77081), and three londranites, Lodran, LEW88280, and MAC88177. In addition, we analyzed LEW88663, which has the bulk composition, mineral chemistry, and oxygen isotopic composition of L-chondrites, but is metal-free and has an achondrite texture; and Divnoe, a plagioclase-poor, olivine-rich primitive achondrite with an oxygen isotopic composition similar to that of the group IAB iron meteorites. These meteorites show a variety of REE patterns in their constituent phases, and there are consistent differences between acapulcoites and lodranites that are consistent with removal of a LREE- and Eu-enriched melt that is apparently responsible for the low plagioclase content of lodranites.

Davis, Andrew M.↗
NASA NTRS1992

CI chondrite-like clasts in the Nilpena polymict ureilite - Implications for aqueous alteration processes in CI chondrites

Petrographic studies of Nilpena polymict ureilite have revealed the presence of small quantities of carbonaceous chondrite matrix clasts. Detailed electron microprobe and TEM studies show that the chemistry and fine-scale mineralogy of one of these clasts is consistent with CI carbonaceous chondrite matrix. Compared to Orgeuil, the phyllosilicate, sulfide, and oxide mineralogy suggests that the Nilpena clasts may represent a less altered type of CI matrix. It is suggested that increased oxidation and aqueous alteration of Nilpena-type materials could result in the formation of the type of mineral assemblage observed in Orgueil. Increased alteration produces progressive more Mg-rich phyllosilicates and more Fe(3+)-rich iron oxides, such as ferrihydrite. As a function of increased alteration, Ca is also progressively leached from the matrix material to form carbonate veins. The depletion of Ca in CI chondrite matrices suggests the Ivuna and Alais may be intermediate in their degree of alteration to Nilpena and Orgueil.

Brearley, Adrian J.↗
NASA NTRS1991

The Carlisle Lakes-type chondrites - A new grouplet with high Delta(17)O and evidence for nebular oxidation

The petrogenesis of the Carlisle Lakes-type chondrites and their relationship to other chondrites are studied using new petrologic data, especially on mineralogical zoning patterns, and oxygen isotopic analyses of the whole chondrites and some of chondrules. Detailed zoning profiles of mafic silicates are measured in order to determine the environment(s) in which their oxidation states are established. It is concluded that the zoning did not form during crystallization from a melt droplet chondrule but post-dated chondrule formation. Parent-body thermal metamorphism and nebular gas-solid exchange reactions accompanied by condensation of new FeO-rich olivine, utilizing existing olivine surfaces as nucleation sites are considered as hypotheses explaining the zoning. The occurrence of zoned grains in a host that is mainly equilibrated suggests that the equilibration of the Carlisle Lakes-type chondrites occurred prior to final lithification.

Weisberg, Michael K.↗
NASA NTRS1991

Chromite and olivine in type II chondrules in carbonaceous and ordinary chondrites - Implications for thermal histories and group differences

Unequilibrated chromite and olivine margin compositions in type II chondrules are noted to differ systematically among three of the chondrite groups, suggesting that type II liquids differed in composition among the groups. These differences may be interpreted as indicators of different chemical compositions of the precursor solids which underwent melting, or, perhaps, as differences in the extent to which immiscible metal sulfide droplets were lost during chondrule formation. Because zinc is detectable only in type II chromites which have undergone reequilibration, the high zinc contents reported for chondritic chromites in other studies probably reflect redistribution during thermal metamorphism.

Johnson, Craig A.↗
NASA NTRS1990

Dark inclusions in Allende, Leoville, and Vigarano - Evidence for nebular oxidation of CV3 constituents

The origin and the history of dark inclusions (DIs) are investigated using petrologic, chemical, and oxygen isotopic data on ten DI samples from Allende, Leoville, and Vigarano. These data indicate that the DIs of the Leoville and Vigarano are closely similar to those of Allende. The inclusions appear to be fragments of CV3 parent bodies which were processed to different degrees prior to their incorporation as clasts into the Allende, Leoville, and Vigarano chondrites. The processing homogenized the olivine compositions, presumably through heating, and also involved oxygen exchange with O-16-poorer surroundings.

Johnson, Craig A.↗
NASA NTRS1988

Petrology of ALH85085 - A chondrite with unique characteristics

The characteristics of the chondrite ALH85085 are examined. It is found that the chondrules of ALH85085 are 25-75 microns in size. The majority of the chondrules are cryptocrystalline and all of them are volatile depleted. It is shown that the FeNi metal abundance is 40.9 wt pct and the sulfide abundance is 1.1 wt pct. The matrix lumps and bulk composition of ALH85085 are analyzed. The characteristics of ALH85085 are compared with other chondrite groups, showing that it cannot be classified. The possible origin of ALH85085 is analyzed, showing trends similar to those of calculated nebular condensation paths indicating a nebular origin.

Weisberg, Michael K.↗
NASA NTRS1988

Cumberland Falls chondritic inclusions. III - Consortium study of relationship to inclusions in Allan Hills 78113 aubrite

The contents of Ag, Au, Bi, Cd, Co, Cs, Ga, In, Rb, Sb, Se, Te, Tl, U, and Zn in large chondritic clasts from the Cumbersand Falls aubrite were determined by radiochemical neutron activation analysis, and the results, together with the results of a mineralogical investigation, were compared with respective data obtained for three primitive inclusions from the ALH A78113 aubrite. The results indicated that the clasts from both aubrite sources constitute a single chondritic suite. The analyses data, together with the results of thermoluminescence data for Cumberland Falls chondritic inclusions and achondritic host, indicate that inclusions in Cumberland Falls and in ALH A78113 aubrite represent a primitive chondrite sample suite whose properties were established during primary nebular accretion and condensation over a broad redox range.

Lipschutz, Michael E.↗