A5030933287- Planetary Science and Exploration
- Astro and Planetary Science
- Space Exploration and Technology
- Space Science and Extraterrestrial Life
- Geology and Paleoclimatology Research
- Solar and Space Plasma Dynamics
- Space exploration and regulation
- Geological and Geochemical Analysis
- Methane Hydrates and Related Phenomena
- Geochemistry and Geologic Mapping
- Spaceflight effects on biology
- Hydrocarbon exploration and reservoir analysis
- Magnetic and Electromagnetic Effects
- Isotope Analysis in Ecology
- Geophysics and Gravity Measurements
- Atmospheric and Environmental Gas Dynamics
- Geomagnetism and Paleomagnetism Studies
- Geological Formations and Processes Exploration
- Paleontology and Stratigraphy of Fossils
- Ancient and Medieval Archaeology Studies
- Dark Matter and Cosmic Phenomena
- Marine and environmental studies
- Particle Detector Development and Performance
- Pleistocene-Era Hominins and Archaeology
- Geological formations and processes
Planetary Science Institute
2019-2023
Memorial University of Newfoundland
2023
Marshall Space Flight Center
2023
Goddard Space Flight Center
2023
University of Colorado System
2023
Johns Hopkins University Applied Physics Laboratory
2023
Kyoto University
2023
University of Iowa
2023
Nagoya University
2023
Los Alamos National Laboratory
2023
[1] The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement composition at fine spatial scales over the full lunar surface. To these objectives, broad spectral with high uniformity and signal-to-noise ratio capable measuring compositionally diagnostic absorption features from variety known possible materials required. For this purpose designed developed that measures 430 3000 nm 10 sampling through 24...
[1] High-resolution compositional data from Moon Mineralogy Mapper (M3) for the Moscoviense region on lunar farside reveal three unusual, but distinctive, rock types along inner basin ring. These are designated "OOS" since they dominated by high concentrations of orthopyroxene, olivine, and Mg-rich spinel, respectively. The OOS occur as small areas, each a few kilometers in size, that widely separated within highly feldspathic setting rim. Although abundance plagioclase is not well...
[1] Analysis of two absorption features near 3 μm in the lunar reflectance spectrum, observed by orbiting M3 spectrometer and interpreted as being due to OH H2O, is presented, results are used discuss processes producing these molecules. This analysis focuses on dependence absorptions physical properties, including composition, illumination, latitude, temperature. Solar wind proton-induced hydroxylation proposed creation process, its products could be a source for other reported types...
We examined the lunar swirls using data from Moon Mineralogy Mapper (M 3 ). The improved spectral and spatial resolution of M over previous imaging facilitates distinction subtle differences, provides new information about nature these enigmatic features. characterized features swirls, interswirl regions (dark lanes), surrounding terrain for each three focus regions: Reiner Gamma, Gerasimovich, Mare Ingenii. used Principle Component Analysis to identify spectrally distinct surfaces at...
[1] The Moon Mineralogy Mapper (M3) provided the first global hyperspectral data of lunar surface in 85 bands from 460 to 2980 nm. Clementine mission multispectral maps 11 spectral across ultraviolet-visible (UV-VIS) and near-infrared (NIR). In an effort understand how M3 improves our ability analyze interpret data, we compare spectra with those Clementine's UV-VIS NIR cameras. NIR. We have found that reflectance values are lower all wavelengths compared albedos both show be redder, is, a...
Abstract The Orientale Basin is one of the largest (930 km diameter) and youngest (~3.8 Ga) impact craters on Moon. As basin only partly flooded by mare lava, its floor materials expose a major portion melt sheet, which some previous work has suggested might have undergone igneous differentiation. To test this idea, we remapped geology using images topography from Lunar Reconnaissance Orbiter, mineralogical information Chandrayaan‐1 Moon Mineralogy Mapper, elemental concentration maps...
Abstract The Schrödinger basin on the lunar farside is ∼320 km in diameter and best-preserved peak-ring of its size Earth–Moon system. Here we present spectral photogeologic analyses data from Moon Mineralogy Mapper instrument Chandrayaan-1 spacecraft Lunar Reconnaissance Orbiter Camera (LROC) LRO spacecraft, which indicates peak ring composed anorthositic, noritic troctolitic lithologies that were juxtaposed by several cross-cutting faults during formation. Hydrocode simulations indicate...
Research Article| December 01, 2023 Space Weathering At The Moon Brett W. Denevi; Denevi Johns Hopkins University Applied Physics Laboratory, 11100 Road, Laurel, Maryland, 20723, U.S.A. brett.denevi@jhuapl.edu Search for other works by this author on: GSW Google Scholar Sarah K. Noble; Noble NASA Headquarters, 300 Hidden Figures Way, SW, Washington, D.C., 20546, sarah.noble-1@nasa.gov Roy Christoffersen; Christoffersen Jacobs, Mail Code XI3, Johnson Center, Houston, Texas, 77058,...
Abstract The Moon Mineralogy Mapper (M 3 ) on the Chandrayaan-1 spacecraft provided nearly global 0.5–3 μ m imaging-spectroscopy data at 140 pixel –1 in 85 spectral bands. Targeted locations were imaged 70 and higher resolution. These enable a detailed look mineralogy, hydroxyl, water signatures exposed lunar surface. We find evidence for multiple processes, including probable solar wind implantation, excavation of hydroxyl-poor water-poor material cratering events, hydroxyl water-rich...
Abstract A strategy for planetary exploration using a rover capable of science autonomy is presented. We encoded into set driving hypotheses pertaining to the geologic origin field site and equipped with instrumentation needed measure observables related hypotheses, as well software tools analyze them relatively high level confidence. investigated effects different strategies that make use compared operational efficiency yield three geological scenarios: (1) standard human-directed...
High‐alumina (HA) mare basalts are a unique group of the lunar sample collection. Sample geochemistry indicates that these derived from sources composed late‐stage cumulates Lunar Magma Ocean (LMO). Their aluminous nature suggests their contained significant plagioclase, which has implications regarding efficiency plagioclase separation earlier forming, mafic in LMO to form anorthositic crust, and hence heterogeneity mantle. The Apollo Luna missions sampled HA four different locations...
Research Article| December 01, 2023 Surface Volatiles on the Moon Dana M. Hurley; Hurley Johns Hopkins University Applied Physics Laboratory, 11100 Road, Laurel, Maryland 20723, U.S.A. dana.hurley@jhuapl.edu Search for other works by this author on: GSW Google Scholar Matthew A. Siegler; Siegler Planetary Science Institute, 1700 E Fort Lowell Rd STE 106, Tucson, Arizona 85719, msiegler@psi.edu Joshua T. S. Cahill; Cahill joshua.cahill@jhuapl.edu Anthony Colaprete; Colaprete NASA Ames Center,...
In this paper, we report analysis of various basaltic lunar samples including 14053 and 14072, KREEP basalt 15386, thirty clasts from Apollo 14 breccia 14321, as well impact-generated (matrix 14168, olivine vitrophyres 14321,1180 14321,1539, impact melt 14310) using a combination solution laser ablation inductively coupled plasma mass spectrometry (ICP-MS). The clast were previously analyzed by instrumental neutron activation. On plots incompatible trace elements (ITEs) vs. compatible...
ABSTRACT Investigation of the lunar crustal magnetic anomalies offers a comprehensive long-term data set observations small-scale fields and their interaction with solar wind. In this paper review mini-magnetospheres is compared quantifiably theoretical kinetic-scale plasma physics 3D particle-in-cell simulations. The aim to provide complete picture all aspects phenomena show how from different international missions interrelate. analysis shows that simulations are consistent formation...
Research Article| December 01, 2023 The Dust, Atmosphere, and Plasma at the Moon William M. Farrell; Farrell NASA Goddard Space Flight Center 8800, Greenbelt Road, Greenbelt, MD, 20771 USA Search for other works by this author on: GSW Google Scholar Jasper S. Halekas; Halekas Department of Physics Astronomy, University Iowa, Iowa City, IA, 52242 Mihaly Horányi; Horányi Physics,University Colorado, Boulder, CO 80309, Rosemary Killen; Killen Cesare Grava; Grava Southwest Institute, 6220...
[1] The Moscoviense Basin, on the northern portion of lunar farside, displays topography with a partial peak ring, in addition to rings that are offset southeast. These do not follow typical concentric ring spacing is recognized other basins, suggesting they may have formed as result an oblique impact or perhaps multiple impacts. In unusual present, Basin contains diverse mare basalt units covering basin floor and few highland mafic exposures within its rings. New analysis previously mapped...
Abstract This paper discusses the methodology and results of a detailed investigation Mare Frigoris using remote sensing data from Clementine, Lunar Prospector, Reconnaissance Orbiter, with objective mapping characterizing compositions eruptive history its volcanic units. With exception two units in west, Lacus Mortis are filled basalts having low‐TiO 2 to very low TiO , low‐FeO, high‐Al O 3 abundances. These indicate that most basalts—a potentially undersampled, yet important group lunar...
Gas-rich discharges of magma produced pyroclastic vents on the lunar surface. Calculations suggest those repeatedly generated 1012 to 1015 g H2O and CO + CO2 for volumes 10 500 km3 early in history, particularly during first billion years history. Some volatiles migrated poles where they could be trapped permanently shadowed regions (PSRs). The largest indigenous source south polar region was volcanism that occurred floor Schrödinger impact basin. Here a large vent ceased erupting ∼ 3.70...
Abstract The diameter range of 15 to 20 km is within the transition from simple complex impact craters located on Moon. This spans roughly a factor 3 in energy for same impactor speed, composition, and trajectory angle. We analyzed global population well‐preserved this size order assess effects target properties crater shapes morphologies. observed that narrow range, are confined highlands, more abundant mare. found unusually deep around highlands‐mare boundaries favor hypothesis they form...
Understanding the origin and evolution of lunar volatile system is not only compelling science, but also fundamental Solar System science. This white paper (submitted to US National Academies' Decadal Survey in Planetary Science Astrobiology 2023-2032) summarizes recent advances our understanding volatiles, identifies outstanding questions for next decade, discusses key steps required address these questions.