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Low molecular weight functionalized polyolefins are mainly used as additives in adhesive formulations, compatibilizing agents and aqueous dispersions. However, the low viscosity and functionality they offer has never been explored to generate high molecular weight products that offer improved processing routes for polyolefins as well as wider applications. The aim of this thesis work was to investigate the preparation and characterization of thermoset material by reactions between a highly functionalized, low viscosity maleic anhydride grafted polyethylene and diamines. Reactions were performed both in solution and in the melt state to generate the target thermoset materials. Products from these reactions were extensively explored using different techniques to understand the reaction kinetics and mechanism. Thermosets generated were also characterized for the degree of crosslinking, thermal, mechanical and thermomechnical properties. Reactions in solution showed that the degree of reaction could be easily controlled by manipulating the concentration of reactants in the reaction mixture. Mixing torque data from the melt blender generated during reactions in the melt phase suggested that reaction between anhydride and amine moieties in these systems happen at much slower rate than widely reported for conventional high molecular weight polymeric systems. Unlike a single or two closely merged peaks in mixing torque associated with melting of polymer and chain extension and crosslinking due to reaction between anhydride and amine functionality widely reported, two separate peaks were observed in this study. A combination of FTIR and insoluble fraction data generated suggested that the first peak observed in mixing torque represents a combination of melting and partial reaction between anhydride and amine functionality. Whereas, the second peak in the mixing torque represents the initiation of crosslinking. The slower kinetics observed in the current inve, Doctor of Philosophy (PhD)

The formation of a polycrystalline solid compact, by fusing an initially porous aggregate of diamond crystals under dynamic shock pressure (7.5–18 GPa), is shown to depend critically on the size of the initial crystals. Porous aggregates of 100–150 µm diameter crystals upon shock compaction produced compacts. These exhibited pronounced fracturing of the individual crystals and showed no evidence of fusion. Aggregates consisting of ultrafine crystals (<5 µm) also exhibited minimal consolidation. However, samples composed of crystals in the range 4–8 µm produced strong fused compacts of polycrystalline diamond. A model calculation indicates that at 10 GPa less than 0.07 mass fraction of the diamond powder can be melted and this molten material is quenched in 0.8 ns for 8-µm-diam crystals.

The production of fused compacts of polycrystalline diamond was achieved by subjecting porous (35%–49% porosity) mixtures of diamond crystals plus graphite (13–16 wt. %) to dynamic shock pressures of 10–18 GPa. The recovered material from an initial mixture of 4–8-µm diamond crystals plus graphite revealed a very homogeneous texture with little evidence of original grain boundaries. The preconsolidation addition of graphite also allowed ultrafine (<5 µm) diamond crystals to be consolidated; this was not previously possible with the use of diamond crystals alone. The results are consistent with calculations which suggest that a thin layer of graphite surrounding a diamond crystal delays thermal equilibrium between the surface and interior of the diamond crystal, thus allowing greater surface heating. Consolidation is also probably enhanced by conversion of graphite to diamond, possibly via the liquid state.

Space weathering is now generally accepted to modify the optical and magnetic properties of airless planetary regoliths such as those on the Moon and Mercury. Under micrometeorite and ion bombardment, ferrous iron in such surfaces is reduced to metallic iron spheres, found in amorphous coatings on almost all exposed regolith grains. The size and number distribution of these particles and their location in the regolith all determine the nature and extent of the optical and magnetic changes. These parameters in turn reflect the formation mechanisms, temperatures, and durations involved in the evolution of the regolith. Studying them in situ is of intrinsic value to understanding the weathering process, and useful for determining the maturity of the regolith and providing supporting data for interpreting remotely sensed mineralogy. Fine-grained metallic iron has a number of properties that make it amenable to magnetic techniques, of which magnetic susceptibility is the simplest and most robust. The magnetic properties of the lunar regolith and laboratory regolith analogues are therefore reviewed and the theoretical basis for the frequency dependence of magnetic susceptibility presented. Proposed here is then an instrument concept using multi-frequency measurements of magnetic susceptibility to confirm the presence of fine grained magnetic material and attempt to infer its quantity and size distribution. Such an instrument would be invaluable on a future mission to an asteroid, the Moon, Mercury or other airless rocky Solar System body.

Space weathering is now generally accepted to modify the optical and magnetic properties of airless planetary regoliths such as those on the Moon and Mercury. Under micrometeorite and ion bombardment, ferrous iron in such surfaces is reduced to metallic iron spheres, found in amorphous coatings on almost all exposed regolith grains. The size and number distribution of these particles and their location in the regolith all determine the nature and extent of the optical and magnetic changes. These parameters in turn reflect the formation mechanisms, temperatures, and durations involved in the evolution of the regolith. Studying them in situ is of intrinsic value to understanding the weathering process, and useful for determining the maturity of the regolith and providing supporting data for interpreting remotely sensed mineralogy. Fine-grained metallic iron has a number of properties that make it amenable to magnetic techniques, of which magnetic susceptibility is the simplest and most robust. The magnetic properties of the lunar regolith and laboratory regolith analogues are therefore reviewed and the theoretical basis for the frequency dependence of magnetic susceptibility presented. Proposed here is then an instrument concept using multi-frequency measurements of magnetic susceptibility to confirm the presence of fine grained magnetic material and attempt to infer its quantity and size distribution. Such an instrument would be invaluable on a future mission to an asteroid, the Moon, Mercury or other airless rocky Solar System body.