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Nagle, J. S.

Publications and source records attributed to Nagle, J. S..

11 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1982

Core segment 15008 - Regolith stratigraphy at Apennine Front Station 2 using multispectral imaging

High precision multispectral images for Apennine Front core segment 15008 are presented. These data have a spatial resolution less than approximately 0.5 mm and are analyzed for their compositional information using image analysis techniques. The stratigraphy of the regolith sampled by 15008 is documented here as three distinct zones, the most prominent of which is a feldspathic fragment-rich zone with a chaotic fabric that occurs between 10 and 18 cm depth. It is suggested that this material is the primary rim crest deposit of the local 10 m crater. Above this zone the stratigraphy is more horizontal in nature. Below this zone the soil is observed to be relatively homogeneous with no distinctive structure to 23 cm depth.

Pieters, C. M.↗
NASA NTRS1982

Depositional history of core 15008/7 - Some implications regarding slope processes

Structures and associated vertical changes in lithology of core 15008/7 are discussed with a view to providing data for interpretation of regolith-forming and accumulation processes that can take place on a continuous slope upon an impact-dominated surface. The light-colored soil between 49.1 and 55.6 cm in core 15007 is rich in clasts which contain abundant green glass and appears to be ejecta from downslope. The dark massive soils between 17.5 and 49.1 cm contain many crater bottom structures and crater fill, but apparently no rim-crest or proximal ejecta. The higher parts of the crater deposits appear to be removed by erosion, whereas the crater fill is preferentially preserved. Such material may be typical of slope deposits. The light-colored soil with contorted, friable clasts, between 0 and 17.5, appears to be ejecta from the crater seen in the sampling photographs.

Nagle, J. S.↗
NASA NTRS1980

Possible rim crest deposits in cores 12027 and 15008 - Some interpretations and problems for future research

Light colored coarse grained soils in the upper parts of cores 12027 and 15008 have a chaotic fabric and abundant bedrock-derived rock fragments. They overlie dark colored, fine grained soils with horizontal fabric and abundant regolith-derived rock fragments. The light colored soils are interpreted to be rim crest deposits associated with the craters seen in the lunar surface sampling photographs. The coarse size, poor sorting and chaotic fabric are believed to have originated by the violent mixing processes which are expected with ejecta deposition. The increase in bedrock-derived particles within the light colored soil can be explained by ejecta from craters that penetrated through or deep into the regolith. The dark soils are believed to predate the craters. Distribution of rock fragments in the material interpreted as rim crest ejecta does not fit a simple model of overturned stratigraphy.

Nagle, J. S.↗
NASA NTRS1980

Multispectral imaging of the lunar regolith core samples - Preliminary results for 74002

Multispectral images of a lunar core segment are a new form of continuous data along the length of the core. A new laboratory arrangement was developed to obtain these images. Data processing and initial data analysis for core section 74002 were performed. The images are sensitive to variations in mineralogy and/or maturity of the soil and are easily used (1) in stratigraphic studies of the lunar regolith, (2) for sample selection of representative material, and (3) as ground truth for remote sensing studies.

Pieters, C. M.↗
NASA NTRS1979

Preliminary description and interpretation of Apollo 14 cores 14211/10

Core 14211/10 is a 2 cm-diameter double drive tube that was collected within the smooth plains area of the Apollo 14 landing site. Rock fragments in the core appear to be derived from the smooth plains area because the coring site is beyond ejecta range of Cone Crater and is within the expected continuous ejecta of two large craters in the plains. The characteristics of the glassy soil breccia zone between 12.5 and 15.5 cm indicate that this zone represents the bottom of a glass-lined crater. At least some of the dark agglutinate and glass-rich soils at the top of the core are mature, by FMR measurements, and show maturation interrelationships between particle types. Hence, this dark interval is interpreted as a gardened zone.

Nagle, J. S.↗
NASA NTRS1975

Stratification in the lunar regolith - A preliminary view

Although our knowledge of lunar regolith stratification is incomplete, several categories of thick and thin strata have been identified. Relatively thick units average 2 to 3 cm in thickness, and appear surficially to be massive. On more detailed examination, these units can be uniformly fine-grained, can show internal trends, or can show internal variations which apparently are random. Other thick units contain soil clasts apparently reworked from underlying units. Thin laminae average approximately 1 mm in thickness; lenticular distribution and composition of some thin laminae indicates that they are fillets shed from adjacent rock fragments. Other dark fine-grained well-sorted thin laminae appear to be surficial zones reworked by micrometeorites. Interpretations of stratigraphic succession can be strengthened by the occurrence of characteristic coarse rock fragments and the orientation of large spatter agglutinates, which are commonly found in their original depositional orientation.

Duke, M. B.↗
NASA NTRS1974

Stabilization of lunar core samples

Processing of lunar cores includes: (1) careful dissection for study of loose fines, and (2) stabilization of the residue by peeling and impregnation. The newly developed technique for preparing thin peels of lunar cores requires application of the methacrylate adhesive to a backing strip, before taking the peel. To ensure complete impregnation of the very fine, dry lunar soil, the low-viscosity epoxy, Araldite 506, is gently flowed onto the core, under vacuum.

Nagle, J. S.↗
NASA NTRS1973

Preliminary stratigraphy of the Apollo 15 drill core

The crew of Apollo 15 collected a 242-cm-long core of the regolith developed on the surface of Palus Putredinus (3 deg 39 min 20 sec E, 26 deg 26 min 00 sec N). This core consists of 42 major textural units, which range from a few millimeters to 13 cm thick. The regolith at this site was deposited layer by layer, each layer having been reworked, to some degree, by micrometeorite bombardment. The particle composition of six layers for which samples were obtained varies in a random fashion, thus supporting the heterogeneous, layered model of the regolith. The ratio of lithic fragments derived from the Apennine Front to that derived from the mare surface is about 1:1. This lithic ratio, in a regolith section 3.75 km from the base of the front, is an indication of the efficiency of lateral transport of soil by impact processes and mass wasting.

Heiken, G.↗
NASA NTRS1972

Stratigraphy of the Apollo 15 drill core

The crew of Apollo 15 collected at 242-centimeter-long core of the regolith of the moon developed on the surface of Palus Putredinis 3 deg 39 min 20 sec E, 26 deg 26 min 00 sec N. The 2.04-centimeter-diameter core, which has a mass of 1333.2 grams, consists of 42 major textural units, with thicknesses ranging from a few milliliters to 13 centimeters thick. The regolith is not homogeneous and is composed of many layers that are mostly ejecta from impact events.

Heiken, G.↗
NASA NTRS1972

Apollo 16 special samples, part B

Information is presented concerning special samples which were collected for specific investigations. The methods of sample collection are described along with fillet and core samples.

Hoerz, F.↗