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• W319166821 abstract "The South Pole–Aitken Basin Sample-Return mission concept (SPA-SR) was highly ranked by the NRCNAS Decadal Survey [1] because the science objectives address Solar-System issues as well as the Earth-Moon system and Moon, specifically. Key objectives relate to (1) the timing and nature of post-accretional bombardment in the inner Solar System by very large objects and subsequent effects on planetary evolution and processes, and (2) planetary differentiation and crustal evolution in general [see also 2,3]. The impact process is among the most fundamental processes in shaping and altering the early-formed surfaces and atmospheres of planets in the inner Solar System. Direct dating and isotopic modeling of Apollo rocks and meteorites has revealed much of the early chronology, yet the timing of the largest and oldest impact structures remains poorly constrained. Constraining the age of SPA either by direct dating of a remnant of its impact melt or by establishing the range of ages of smaller, subsequently formed basins within SPA, will increase knowledge of how, when, and why these massive impacts occurred and how they affected early surfaces and surface environments of the terrestrial planets. The Moon is key to understanding the early history of planet formation and differentiation into crust, mantle, and core because its rocks and minerals retain a direct record of its primary crust. It cooled quickly, so crust-mantle processing has not been extensive. The Moon is the well-studied small-planet endmember that allows us to understand relationships between a planet’s size and composition, and how it cooled, differentiated, and was subsequently modified by internally generated igneous and volcanic processes. Much of what is well known about the Moon stems from the analysis of samples and data collected from a relatively small area and fraction of the Moon’s Earth-facing side. Recent global remote sensing shows the Moon to be significantly more diverse than is reflected by the samples now in hand. The SPA basin lies far from the sampled near-side locations, and the impact that produced it excavated materials from deep in the crust or upper mantle. Thus, we expect samples from SPA basin to provide significant new insight into early planetary differentiation. Additional specific objectives of SPA-SR are pivotal for lunar science [1] and foundational for understanding processes important during early planetary differentiation. These include, but are not limited to, the following: determine composition and mineralogy of lower crust directly from samples (test models for differentiation of the Moon’s crust and mantle); determine composition and mineralogy of the mantle beneath SPA; calibrate/validate compositional and mineralogic remote sensing over a major part of the Moon (SPA) where existing data are ambiguous or otherwise not well understood and for which no samples are known to exist in Apollo, Luna, or meteorite collections (enabling improved understanding of the lunar surface and bulk composition); obtain materials that are less likely than existing samples to be biased by the youngest and largest near-side impact basins (e.g., Serenitatis, Imbrium); determine sources of anomalous concentrations of thorium and other heat-producing elements to understand lunar differentiation and thermal evolution, including volcanism; determine ages and compositions of basalts to reveal if the mantle source regions on the far side of the Moon and timing of volcanism differ from regions previously sampled. In this abstract we discuss approaches and measurements to be made on returned samples to address these objectives. Over thirty years of experience exist for the analysis of lunar materials; in some cases, however, new equipment now permits analyses that were not possible during much of that time. Noteworthy are capabilities for microanalysis that have been and continue to be developed for the investigation of small planetary samples and cosmic dust [e.g., 4 and refs therein]. Much can be done with small rock samples that was not possible or routine until recently, such as in-situ micro-isotopic and geochemical analyses using new/improved methods such as SIMS, LA-ICPMS, MC-ICPMS, SXRF, PIXE, and others [see 4]. Furthermore, much of what can now be done has not been done extensively with existing small rock fragments from the lunar regolith because of the availability of the large Apollo rock samples. Well-established analytical approaches have nevertheless been used effectively for many years on small lunar rock fragments (e.g., SIMS, EMP, INAA, XRF, SEM, TEM), and those results are just as pertinent to samples from an SPA-SR. Geochronology. Fundamentally important to SPASR science goals is the capability to determine ages of small and in most cases complex (breccia) samples. The goal of assigning an absolute age to the SPA event can be attained with varying degrees of confidence by direct and indirect means. This goal would be achieved directly by dating a sample of the original crystallized impact melt; such a sample is not necessary to obtain this goal, however. Clasts of crystalline impact melt that were incorporated into later-formed breccias can be extracted and dated [5]. Crystalline impact melt produced by proximal post-SPA basins can be dated to provide constraints. If multiple basin-forming events are dated, SPA would logically be at least as old as the oldest one. Post-SPA volcanic rocks will also contribute to" @default.
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• W319166821 date "2003-03-01" @default.
• W319166821 modified "2023-09-23" @default.
• W319166821 title "Scientific Expectations from a Sample of Regolith and Rock Fragments from the Interior of the Lunar South Pole-Aitken Basin" @default.
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