What is ejecta plume

Wittmann, T. Kenkmann, L. Hecht, D. GSA Bulletin ;; : — The temporal evolution of the cratering process from the initial stage of excavation to the collapse of the ejecta plume is evidenced by the petrographic characteristics and modal composition of the suevitic rocks, including the size distribution and shape parameters of melt particles. Emplacement of the lowermost suevitic deposits likely started in the first minute after the impact by the passing ejecta curtain that interacted with the expanding ejecta plume.

On top of this brecciated impact melt rock, the collapsing ejecta plume deposited air-fall suevites. The basal air-fall unit, Middle Suevite, may have been deposited due to a density current—like clumping of hot debris. With progressive cooling, regions of the ejecta plume were entrained in its collapse that produced vapor condensates, accretionary rims, and different oxygen fugacities.

After cooling progressed, atmospheric conditions began to reestablish over the crater and turbulence decreased, supposedly after the first 10 min of initial ejecta plume collapse. This led to a winnowing out of fine matrix material and distinct sorting. Shibboleth Sign In. OpenAthens Sign In. Institutional Sign In. Sign In or Create an Account. User Tools. Sign In. Advanced Search. Skip Nav Destination Article Navigation. Close mobile search navigation Article navigation.

Volume , Number Publication Type. More Filters. Preliminary laboratory investigations of ejecta emplacement dynamics and morphology with planetary applications. Abstract The preponderance of impact craters and the associated crater ejecta facies are leading agents of geomorphic change across the Solar System. Interpretation of planetary landscape evolution, … Expand. Physical characterization of a simulated impact-vapor plume using laser ablation of Chicxulub sediments.

Abstract An asteroid impacted the Yucatan carbonate platform in the Southern Gulf of Mexico about 66 million years ago. The ejecta and impact-vapor plume introduced massive amounts of gases and dust … Expand.

Report on modelling and simulations of NEO response to deflection attempts. Abstract Of the several near-Earth and Main Belt asteroids visited by spacecraft to date, three display a paucity of small craters and an enhanced number of smoothed and degraded craters: Eros, … Expand.

View 4 excerpts, cites methods, results and background. Abstract An understanding of the post-impact dynamics of ejecta clouds are crucial to the planning of a kinetic impact mission to an asteroid, and also has great implications for the history of … Expand.

View 1 excerpt. Size of particles ejected from an artificial impact crater on asteroid Ryugu. A projectile accelerated by the Hayabusa2 Small Carry-on Impactor successfully produced an artificial impact crater with a final apparent diameter of Fates and evolutionary dependencies.

Abstract This paper presents a quantitative study of the evolution of the ejecta cloud released from a hypervelocity impact on a binary asteroid. View 1 excerpt, cites methods. This investigation … Expand. View 4 excerpts, cites background and methods. An N-body approach to modelling debris and ejecta off small bodies: implementation and application. We introduce here our new approach to modeling particle cloud evolution off surface of small bodies asteroids and comets , following the evolution of ejected particles requires dealing with various … Expand.

View 2 excerpts, cites background and methods. Mars impact ejecta in the regolith of Phobos: Bulk concentration and distribution. Abstract The gravity of Mars and the observation of a thick Phobos regolith suggest that nearly all Phobos ejecta returns to Phobos and re-impacts on Phobos.

Primary ejecta from Mars typically … Expand. Highly Influenced. View 5 excerpts, cites background. A ballistics analysis of the Deep Impact ejecta plume: Determining Comet Tempel 1's gravity, mass, and density. In this work, we develop a first-order, … Expand. View 1 excerpt, references background. Introduction: Planetary impacts occur primarily at nonvertical angles, and craters that form from the lowest impact angles have an uprange forbidden zone in the ejecta that appears as an outward … Expand.

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