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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.
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Numerical Simulations of Laboratory‐Scale, Hypervelocity‐Impact Experiments for Asteroid‐Deflection Code Validation
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Optical and acoustic ground effects simulations from terminal defense asteroid disruption via the PI method
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Asteroid deflection: Do multiple impacts from a split-impactor increase total momentum transfer?
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Hayabusa2 extended mission target asteroid 1998 KY26 is smaller and rotating faster than previously known
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Asteroids for ultralight dark-photon dark-matter detection
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Maximal gravitational wave signal from asteroid-mass primordial black hole mergers at resonant microwave cavities
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The Pecora Escarpment (PCA) 91020 EL3 chondrite and deformation on the EL3 asteroid
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Planetary Defense: Asteroids, Comets, Impact Craters, and Outwitting the Dinosaurs
Abstract not provided.
Planetary Defense: Using Supercomputers to Prevent Asteroid Impacts on Earth [Slides]
Abstract not provided.
Prospect for cislunar spacecraft and near-earth asteroid detection using heliostat fields at night
presentation to accompany recently approved manuscript for SPIE Paper 13149-66 under IR tracking number 1752319
Quantifying asteroid impact energy: Implications for planetary defense (press conference panel)
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Nuclear Deflection of Kilometer-Scale Asteroids Simulated using Sandia's Z Machine
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High-Fidelity Simulation of Asteroid Airbursts at LLNL
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Constraints on Chondrule Generation, Disk Dynamics, and Asteroid Accretion from the Compositions of Carbonaceous Meteorites
The elemental and isotopic compositions of meteorites are expected to reflect several key processes that occurred in the early solar system, including the migration of gas and dust throughout the protoplanetary disk, the formation of chondrules, and the accretion of the first planetary bodies. However, the specific origins of the various compositions measured among these rocks are currently poorly constrained, limiting our understanding of these processes. Here, we use previously measured elemental and isotopic compositions of chondrites and iron meteorites to identify that carbonaceous (CC) meteorites are mixtures of noncarbonaceous (NC) material, calcium–aluminum-rich inclusion (CAI) material, and CI (Ivuna-like) material, in varying proportions. These trends indicate that chondrules in CO (Ornans-like), CM (Mighei-like), CV (Vigarano-like), and TL (Tagish Lake) chondrites share near-identical average proportions of CI material, arguing that they were generated through the remelting of preexisting NC chondrules all in the same disk environment. Because this proportion likely evolved over space and time throughout the disk, this similarity argues that these chondrules originate from a restricted spatial region and time interval, favoring their generation through a localized event. Moreover, the compositions of CR (Renazzo-like) chondrites indicate that their constituents formed through mechanisms different from those in CO, CM, CV, and TL chondrites. Furthermore, the recovered proportions of CI material in CC iron meteorites and chondrites together also argue for evolution in either the predominant direction of dust and gas motion in the first ~10 au of the disk or the radial distance of planetesimal accretion throughout the CC reservoir.