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Haggerty, S. E.

Publications and source records attributed to Haggerty, S. E..

33 records · Page 2
All sourcesNASA NTRSDOE OSTI
NASA NTRS1977

Luna 24 - Opaque mineral chemistry of gabbroic and basaltic fragments from Mare Crisium

Spinels and ilmenites are relatively sparse in the Luna 24 gabbro and basalts. Spinel compositions show some affinities to those of spinels in Apollo 12, Apollo 14 and Luna 16 basalts; a characteristic feature is high Al2O3, reaching a maximum of 19.8 wt%. A comparison of spinels in the Luna 24 gabbro with those in other deep-seated lunar intrusive rocks shows a characteristic trend for Fe/Mg. This trend is systematic from gabbro to anorthosite to troctolite and is interpreted to be P-T dependent. Compositions of spinels in the gabbro fall within the Cr/Al trend defined by the spinels of the basalts, but form a Fe/Mg trend parallel to that of the basalts; this relationship suggests that both the gabbro and the basalts are derived from a closely similar source region, with the basalts originating at a slightly greater depth than the gabbro. The spinels in both rock types are considered to have formed at high crustal levels, at low pressures. The Luna 24 data suggest that the compositional discontinuities which exist between chromian spinels and titanian spinels in a large proportion of mare basalts are the result of nucleation of chromian spinels at high crustal levels prior to eruption, and of titanian spinels during melt crystallization at the lunar surface.

Haggerty, S. E.↗
NASA NTRS1977

Apollo 14 - Oxide, metal, and olivine mineral chemistries in 14072 with a bearing on the temporal relationships of subsolidus reduction

One of three primary objectives of the reported study is related to the definition of the distribution of troilite and Fe and the evaluation of the role of FeS in subsolidus reduction assemblages. Another objective was concerned with the definition of the lower limit of stabilizing elements such as Mg, Al, and Cr in ulvospinel to determine the terminal compositions at which reduction is inhibited. The third objective involves a comparison of the mineral chemistries of decomposed olivine with unaltered olivine in an attempt to determine the temperature limits. The sample was selected because it is one of the most intensely reduced samples returned from the moon. The model invoked for reduction is a magmatic-deuteric process which requires an environment approximating that of a closed system in which the volatile constituents are contained and in which reduction proceeds continuously with crystallization.

Haggerty, S. E.↗
NASA NTRS1974

Apollo 17 orange glass - Textural and morphological characteristics of devitrification

Results of a study are presented concerning (1) the significance of nonexcentroradial growth textures in Apollo 17 orange glass and a comparison of these textures with those that develop in lunar and meteoritic chondrules, (2) the development and the nature of the crystalline-glass interface, and (3) the morphology and growth characteristics of olivine and of the opaque mineral oxides that result by devitrification of the orange glass. Observations of the orange glass soil are contrasted with subsequent partial melting of orange glass spherules that were incorporated into mildly metamorphosed breccias, and the quench textures that result in these larger cooling units are compared with the textures produced by supercooling of small particulate spherules. Results show that the expected changes in viscosity due to partial melting and recrystallization do not affect the shape of individual particles, and that neither the thermal gradients that need to be invoked across 20-100 micron spheres nor collision of glass particles during lava fountaining can account for the devitrification textures observed.

Haggerty, S. E.↗
NASA NTRS1973

Ortho and para-armalcolite samples in Apollo 17.

Two paragenetically contrasting forms of armalcolite are present in basalts from the Apollo 17 Taurus-Littrow landing site. These armalcolites differ in optical properties, in crystal habit and in their distribution between coarse and fine grained rocks. It is proposed to call the two armalcolite forms ortho-armalcolite and para-armalcolite. Texural relationships and the evidence of experimental melting show that ortho-armalcolite is always the first crystalline phase to appear from unusually titanium rich magmas. The origin of para-armalcolite is not yet fully understood.

Haggerty, S. E.↗
NASA NTRS1973

Armalcolite and genetically associated opaque minerals in the lunar samples

A comprehensive electron microprobe study of armalcolite in samples from five Apollo sites (11-16), together with analytical data previously reported from Apollo 17 and Luna 20 show that three distinct compositional types of armacolite are present in the lunar samples. These types are classified as armalcolite, Cr-Zr-Ca-armalcolite and Zr-armalcolite. The Zr-free armalcolites are typical of high-Ti mare basalts whereas the Zr-rich armalcolites are typical of non-mare high alumina basalts. The latter armalcolites are in complete oxide intergrowths (baddeleyite, zirconolite, rutile, ilmenite, and chromite) and are in contrast to the Zr-free armalcolites which are commonly only associated with ilmenite. Subsolidus decomposition of armalcolite to an iron and Mg-rich rutile + ilmenite-geikielite, and the solid state formation of armalcolite from magnesium-ilmenite + niobian-rutile are described for the first time in the lunar samples.

Haggerty, S. E.↗
NASA NTRS1972

Luna 16 - An opaque mineral study and a systematic examination of compositional variations of spinels from Mare Fecunditatis.

The opaque mineralogy of the Luna 16 soil sample is studied, with an emphasis on a detailed survey of the compositional variations of the Fe-Ti-Cr-Al-Mg spinels. Analytical data are also presented for ilmenite. Textural characteristics and shock-metamorphic effects on the opaque minerals are briefly described and comparisons are made throughout between the Luna 16 samples and published and unpublished data on the Apollo samples.

Haggerty, S. E.↗
NASA NTRS1971

Subsolidus reduction of lunar spinels.

Discussion of evidence that some lunar basalts must have exceeded the lower limit of crystallization oxygen fugacity (fO2) by several orders of magnitude. The evidence is based primarily on the decomposition of Cr-Al-ulvospinel, and is further supported in one case by the decomposition of olivine. The data suggest that some rocks have undergone intense nonequilibrium subsolidus reduction. The reduction phenomenon is widespread, and is considered to have developed either during initial deuteric cooling or as a result of a postcrystallization reduction event.

Haggerty, S. E.↗
NASA NTRS1971

Compositional variations in lunar spinels.

Electron probe data for spinels from Apollo 11, 12, and 14 are presented and analyzed. A modified Johnstone spinel prism showing the data distribution is given. Three projections of this prism are then presented which illustrate the variations of simple ratios that are present in the prism and permit three different perspectives of the data. The results are summarized as fO2 isobars on the spinel prism.

Haggerty, S. E.↗