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Shih, C.-Y.

Publications and source records attributed to Shih, C.-Y..

At least 91 records · Page 5
All sourcesNASA NTRSDOE OSTI
NASA NTRS1990

Age of eucrite clast from the Bholghati howardite

The age of the 'large' eucrite clast from the Bholghati howardite (described by Reid et al., 1990) was estimated from Ar-39/Ar-40 age data obtained for a portion of this clast. The Ar-39/Ar-40 age and isotopic systematics of the clast are found to be consistent with those of other eucrites and support the assumption of a common parent body for howardites and eucrites. The Ar-39/Ar-40 data and some of the Rb-Sr data show that Bholghati was affected by a major thermal event about 2-3 Ga ago.

Nyqist, L. E.↗
NASA NTRS1989

Chemical and isotopic constraints on the petrogenesis of the large mare basalt clast in breccia 15459

Results are presented that demonstrate that the large mare basalt clast in Apollo 15 breccia 15459 may represent one or more independent magma types. The complex nonequilibrium pyroxene and plagioclase compositions and relatively abundant mesostasis suggest that the 15459 clast is not a slowly cooled crystal cumulate. The addition of about 40 percent olivine to an olivine-normative basalt parental magma is found to be necessary to explain the high MgO abundances of picritic basalts by the accumulation of olivine in the magma. The present clast has a slightly younger age and a slightly higher Sr-87/Sr-86 ratio than most Apollo 15 basalts.

Nyquist, L.↗
NASA NTRS1987

Isotopic analysis of basaltic fragments from lunar breccia 14321 - Chronology and petrogenesis of pre-Imbrium mare volcanism

Internal (mineral) Rb-Sr isochrons were determined for six Apollo 14 mare basalts of lunar breccia 14321. The ages of these fragments, which represent the time of crystallization of the respective mafic lavas, range from about 4.05 to 4.24, and, possibly, to 4.33 Ga and are among the oldest dates reported for mare basalts. For three of the fragments, internal Sm-Nd isochron data were collected and initial Nd isotopic composition was determined. The results are discussed with reference to the original source of these different basaltic fragments.

Dasch, E. J.↗
NASA NTRS1987

Geochronology of high-K aluminous mare basalt clasts from Apollo 14 breccia 14304

Two aluminous mare basalt clasts of high K abundances from Apollo 14 breccia 14304 (the 14304,127 and 14304,128 samples) were characterized with respect to the Rb and Sr concentrations and isotopic compositions, and the Rb-Sr, K-Ar, and Sm-Nd isotopic age determinations were carried out. The results suggest that these high-K basalts were melts derived from mantle material and that they have experienced about ten-fold Rb/Sr and K/La enrichments at approximately the time of crystallization.

Shih, C.-Y.↗
NASA NTRS1986

Rb-Sr and Sm-Nd internal isochron ages of a subophitic basalt clast and a matrix sample from the Y75011 eucrite

Rb-Sr and Sm-Nd dating studies of the Yamato polymict eucrite Y75011, which contains several coarse-grained mesostasis-rich basaltic clasts with subophitic texture which are representative of pristine lavalike basalts extruded on the surface of the Howardite-Eucrite-Diogenite (HED) parent body, are reported. The results show that moderately evolved basaltic lavas were produced very early in the history of the HED parent body. Their preservation as clasts in the polymict eucrites suggests derivation from a different geological setting on the parent body than that occupied by the more thermally metamorphosed monomict eucrites. It is suggested that the preservation of pristine clasts in polymict eucrites may be due to their impact excavation to the surface of the parent body away from heat sources concentrated within impact craters.

Nyquist, L. E.↗
NASA NTRS1986

Geochronology and petrogenesis of Apollo 14 very high potassium mare basalts

Rb-Sr, K-Ar, and Sm-Nd isotopic studies were undertaken for two Apollo 14 very high potassium (VHK) highly radiogenic mare basaltic clasts from breccias 14305 and 14168. Rb-Sr data indicate ages of 3.83 + or - 0.08 b.y., and 3.82 + or - 0.12 b.y. for samples 14305 and 14168 respectively, for lambda(Rb-87) = 0.0 139/b.y. Their corresponding initial Sr-87/Sr-86 ratios are nearly identical, as well as their Ar-39 to Ar-40 age spectra, and it is proposed that they were derived from the same flow. The Sm-Nd isotopic data of whole rock and mineral separates for the two VHK basalts define an internal isochrone age of 3.94 + or - 0.16 b.y. for lambda (Sm-147) = 0.00654/b.y. and an initial Nd-143/Nd-144 of 0.50673 + or - 21. The similarity in isotopic ages suggests that VHK basalts crystallized from a melt about 3.85 b.y. ago. VHK basalts show very large Rb/Sr fractionation but no significant Sm/Nd fractionation at the time of crystallization. The source material had a Rb/Sr ratio similar to those of Apollo 14 high-Al mare basalts and a nearly chrondritic Sm/Nd ratio. Basalt/granite interaction was found to be responsible for the extreme enrichments of Rb/Sr and K/La during the formation of VHK basalts. It is concluded that K, Rb-rich components of granitic wall rocks in the highland crust were selectively introduced into ascending hot high-Al mare basaltic magma upon contact.

Shih, C.-Y.↗
NASA NTRS1985

Very high potassium (VHK) basalt - Complications in mare basalt petrogenesis

The first comprehensive report on the petrology and geochemistry of Apollo 14 VHK (Very High Potassium) basalts and their implications for lunar evolution is presented. The reported data are most consistent with the hypothesis that VHK basalts formed through the partial assimilation of granite by a normal low-Ti, high-Al mare basalt magma. Assimilation was preceded by the diffusion-controlled exchange of alkalis and Ba between basalt magma and the low-temperature melt fraction of the granite. Hypotheses involving volatile/nonvolatile fractionations or long-term enrichment of the source regions in K are inconsistent with the suprachondritic Ba/La ratios and low initial Sr-87/Sr-86 ratios of VHK basalt. An important implication of this conclusion is that granite should be a significant component of the lunar crust at the Apollo 14 site.

Shervais, J. W.↗
NASA NTRS1985

Isotope analysis of crystalline impact melt rocks from Apollo 16 stations 11 and 13, North Ray Crater

The North Ray Crater Target Rock Consortium was formed to study a large number of rake samples collected at Apollo 16 stations 11 and 13 with comparative chemical, mineralogical, and chronological techniques in order to provide a larger data base for the discussion of lunar highland evolution in the vicinity of the Apollo 16 landing region. The present investigation is concerned with Rb-Sr and Sm-Nd isotopic analyses of a number of whole-rock samples of feldspathic microporhyritic (FM) impact melt, a sample type especially abundant among the North Ray crater (station 11) sample collection. Aspects of sample mineralogy and analytical procedures are discussed, taking into account FM impact melt rocks 6715 and 63538, intergranular impact melt rock 67775, subophitic impact melt rock 67747, subophitic impact melt rock 67559, and studies based on the utilization of electron microscopy and mass spectroscopy.

Reimold, W. U.↗
NASA NTRS1985

Chronology and petrogenesis of a 1.8 g lunar granitic clast:14321,1062

Geochronological, isotopic, and trace element data for a pristine granite clast from Apollo 14 breccia 14321 obtained using Rb-Sr, Sm-Nd, and (Ar-39)-(Ar-40) methods are presented. Trace element data for a possibly related evolved rock, the quartz-monodiorite clast from breccia 15404 are also presented, and the relationship between these two rock types is discussed. The concordancy of the Rb-Sr and Sm-Nd internal isochron ages and especially the Rb-Sr model age strongly suggest that the granite clast formed 4.1 AE ago. It probably crystallized slowly in the crust and was later excavated and brecciated about 3.88 AE ago, as indicated by the Ar-Ar age. A two-stage model involving crystal fractionation followed by silicate liquid immiscibility is proposed for the lunar granite genesis.

Shih, C.-Y.↗
NASA NTRS1983

Pre-4.2 AE mare-basalt volcanism in the lunar highlands

The discovery of a 4.23 AE, low-Ti composition mare basalt from the Fra Mauro Formation has challenged the hypothesis that the plutonism of the lunar highlands and the mare-type volcanism are two separate problems in both space and time. Attention is presently given to data indicating that non-KREEPy, mare-type volcanism began at least as early as 4.2 AE in the Fra Mauro region, and probably across much of the lunar surface. Massive bombardment during the 'terminal cataclism', and the subsequent veneer of younger mare basalts has obliterated most of the evidence for these ancient volcanic events, which may be related to such basin-forming events as the impact-triggered igneous activity that made Procellarum.

Taylor, L. A.↗
NASA NTRS1982

Chronology and petrogenesis of young achondrites, Shergotty, Zagami, and ALHA77005 - Late magmatism on a geologically active planet

Three achondrites were examined for chronology, petrogenesis, and relationships among the shergotites. Isotopic and trace elements analyses were carried out through neutron activation and mass spectrometry on Shergotty, Zagami, and ALHA77005 samples. Attention was given the Rb-Sr, Sm-Nd, and the Ar-39/Ar-40 ages in the samples. Evidence was detected for a shock metamorphism and a younger age of the meteorites than with most other achondrites. Depletions of the rare-earth elements were observed in Shergotty and Zagami, and to a more pronounced degree in ALHA77005. The Rb-Sr internal isochrons for all three meteorites were about 180 Myr, while the Ar-39/Ar-40 plateau ages of Shergotty and Zagami maskelynite were determined at 250-260 Myr. No precise identification of the crystallization ages was found. It is suggested that the achondrites originated in a parent body which experienced at least two epochs of sustained melting.

Shih, C.-Y.↗
NASA NTRS1982

A comparative Rb-Sr, Sm-Nd, and K-Ar study of shocked norite 78236 - Evidence of slow cooling in the lunar crust

The sample 78236 was chipped from the top of a norite boulder at Station 8 by the Apollo 17 landing team. Jackson et al. (1975) concluded that this rock formed at a depth of 8-30 km in the lunar crust and suggested that it was excavated by a large basin-forming impact event. A petrographic description of the boulder is provided, and isotopic analyses are discussed. Attention is given to a chronology for 78236 which seems to be most consistent with radiometric and other evidence. It is proposed that cumulate norite 78236 formed deep in the lunar crust approximately 4.4 AE ago. The rock cooled slowly in the crust until it was excavated by a major basin-forming event. Excavation may have occurred about 4.2 AE ago, but the time of this event is not well constrained.

Nyquist, L. E.↗
NASA NTRS1981

Isotopic and REE studies of lunar basalt 12038 - Implications for petrogenesis of aluminous mare basalts

Sr, Nd, and Sm isotopic studies of lunar basalt 12038, one of the so-called aluminous mare basalts, are reported. The evolution of the Sr and Nd isotopic compositions and the rare earth element (REE) abundances is successfully modeled within the framework of the model developed by Nyquist et al. (1977, 1979) for Apollo 12 olivine-pigeonite and ilmenite basalts. It is pointed out that the isotopic and trace element features of 12038 can by modeled as produced by partial melting of a cumulate mantle source which crystallized from a lunar magma ocean with a chondrite-normalized REE pattern of constant negative slope. Chondrite-normalized La/Yb is equal to 2.2 for this hypothetical magma ocean pattern.

Nyquist, L. E.↗
NASA NTRS1979

The Sr and Nd isotopic record of Apollo 12 basalts - Implications for lunar geochemical evolution

Alkali, alkaline earth, and rare earth element data are reported for several Apollo 12 basalts which are representative of the four Apollo 12 magma types. Results confirm the heterogeneity of the lunar mantle and show that the Sm/Nd ratio of at least the Apollo 12 ilmenite basalts was decreased by 13-24% during magma genesis. In addition, whole mare basalt Sm-Nd data are not collinear on an isochron diagram; thus it is no longer possible to explain these data via mixing of 'primitive material' and 'early differentiates' as in the hybridization and assimilation models.

Nyquist, L. E.↗
NASA NTRS1979

Petrology, chemistry, and chronology of Apollo 14 KREEP basalts

The results of petrographic, major and trace element geochemical, and Rb-Sr isotopic studies of four crystalline matrix breccias and two intergranular to subophitic basalts are reported. Emphasis is placed on the relationship of the basalt fragments to other Apollo 14 KREEP basalts, and the origin of this group as a whole. Considering the high siderophile element content, the balance of evidence favors origin of the Apollo 14 KREEP basalts by impact melting, probably a single melt with slight chemical and isotopic heterogeneities.

Mckay, G. A.↗
NASA NTRS1976

Mare basalt genesis - A cumulate-remelting model

In the framework of the cumulative-remelting model of lunar evolution, high-Ti basalts can be produced by extensive melting of a late-stage cumulate consisting of ilmenite-plagioclase-clinopyroxene-olivine at shallow depths immediately beneath about 60 km thick plagioclase-rich crust. Low-Ti mare basalts can be derived by small degrees of partial melting of an earlier cumulate containing mainly olivine-clinopyroxene-orthopyroxene with minor plagioclase or spinel at greater depth.

Shih, C.-Y.↗
NASA NTRS1975

On the origin of high-Ti mare basalts

Analyses were conducted of sixteen Apollo 17 mare basalts for alkali, alkaline-earth, and rare-earth elements, Co, and Sc. The obtained data were utilized in a study concerning the nature of the igneous processes responsible for the chemical variations among the high-Ti, low-K basalts. Estimates were obtained regarding the abundances of the large-ion, lithophile elements in the source regions for the basalts. It is shown that the source regions could plausibly have been produced by processes believed to have occurred during the early history of the moon. Attention is given to chemical variations among the Apollo 17 mare basalts, near-surface (low-pressure) crystal fractionation, partial melting, limits on the extent of partial melting, and a summary of possible events leading to formation of high-Ti mare basalts.

Shih, C.-Y.↗