4 edition of Inversion of crater morphometric data to gain insight on the cratering process found in the catalog.
Inversion of crater morphometric data to gain insight on the cratering process
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va
Written in English
|Statement||Robert R. Herrick and Suzanne N. Lyons.|
|Series||[NASA contractor report] -- NASA/CR-207849., NASA contractor report -- NASA CR-207849.|
|Contributions||Lyons, Suzanne N., United States. National Aeronautics and Space Administration.|
|The Physical Object|
The cratering process will help reveal what type of material makes up the nucleus (or at least the outer layer), and therefore how the comet formed and evolved. If the crater turns out to be gravity-dominated, this lends evidence to the theory that the comet's nucleus consists of porous, pristine, unprocessed material, and that the comet formed. 1. Introduction. Almost all solid bodies in the solar system exhibit impact craters on their surface. Although it is now generally accepted that the heavily cratered landscapes on planetary bodies, e.g. the Moon, testify that impact cratering is an important geological process in the evolution of all planetary bodies (Melosh and Ivanov,), the process of crater formation itself is still not.
Abstract— The lengths of the shadows cast within simple, bowl‐shaped impact craters have been used to constrain their depths on a variety of planetary bodies. This technique, however, only yields the “true” crater depth if the shadow transects the crater center where the floor is deepest. In the past, attempts have been made to circumvent this limitation by choosing only craters where. The formation process for each crater type is illustrated below using computer models. The effects of a number of impact parameters, including impactor size, surface gravity and target temperature, on the cratering process are also highlighted. SIMPLE CRATERS.
sense, impact cratering is the most fundamental geologic process in the Solar System. History of impact crater studies craters were discovered in when Galileo pointed his irst crude telescope at the Moon. Galileo recognized the raised rims and central peaks of these features, but described them. Our best-known example of such a large crater, Meteor Crater in Arizona (), is ab years old. However, the cratering rate can be estimated from the number of craters on the lunar maria or calculated from the number of potential “projectiles” (asteroids and comets) present in the solar system today.
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Inversion of crater morphometric data to gain insight on the cratering process ROBERT R. HERRICK l* AND SUZANNE N. LYONS2t 1Lunar and Planetary Institute, Bay Area Boulevard, Houston, TexasUSA 2Department of Geology and Geophysics, Texas A&M University, College Station, TexasUSA.
Get this from a library. Inversion of crater morphometric data to gain insight on the cratering process. [Robert R Herrick; Suzanne N Lyons; United States.
We present general inversion techniques that can utilize the morphometric data to quantitatively test various models of complex crater formation.
The morphometric data we use in this paper are depth of a complex crater, the diameter at which the depth-diameter ratio changes, and onset diameters for central peaks, terraces, and peak by: 6.
Inversion of crater morphometric data to gain insight on the cratering process. ROBERT R. HERRICK; SUZANNE N. LYONS; Pages: ; First Published: 04 February Inversion of crater morphometric data to gain insight on the cratering process.
morphometric data for Venus and several outer planet satellites have been collected, so we now have. Herrick RR, Lyons SN () Inversion of crater morphometric data to gain insight on the cratering process.
Meteorit Planet Sci – CrossRef Google Scholar Herrick RR, Sharpton VL, Malin MC, Lyons SN, Feely K () Morphology and morphometry of impact craters. Inversion of crater morphometric data to gain insight on the cratering process We present general inversion techniques that can utilize the morphometric data to quantitatively test various.
Herrick R, Lyons S. Inversion of crater morphometric data to gain insight on the cratering process. Meteoritics Planetary Sci ; Meteorite crater - Meteorite crater - The impact-cratering process: When an asteroidal or cometary object strikes a planetary surface, it is traveling typically at several tens of kilometres per second—many times the speed of sound.
A collision at such extreme speeds is called a hypervelocity impact. Although the resulting depression may bear some resemblance to the hole that results from. Request PDF | On Jan 1,Kai Wang Ng published Inversion of Bayes’ Formula for Events | Find, read and cite all the research you need on ResearchGate.
Updated catalogs of peak-ring basins, protobasins, and complex crater ≥50 km. • New morphometric data include depth, areas, circularity, and peak dimensions. • The transition from crater to basin is marked by an abrupt change in morphometry.
• Impact melt was important in modifying crater and basin morphometries. The diameter of an impact crater is one of the most basic and important parameters used in energy scaling and numerical modeling of the cratering process.
However, within the impact and geological communities and literature, there is considerable confusion about crater sizes due to the occurrence of a variety of concentric features, any of. Data inversion schemes based on inflection points, minima and maxima are discussed for SRT and GRT.
data to gain insight on the cratering process. quantitatively test various models of. The term “transient crater” means the cratering process continues after the excavation flow comes to rest.
What happens to the transient crater. This depends on how large the crater is. In the case of small transient craters, modifications are moderate. On relieving of pressure, there is an elastic rebound at the crater floor now hosting a.
1 Introduction. Secondary impact craters form in the fallback collisions of ejecta from primary impacts. Secondary cratering is an important planetary surface process and has implications for estimating surface ages as well as understanding regolith evolution and impact cratering mechanics [McEwen and Bierhaus, ].Some of the earliest studies of low‐energy impacts involved laboratory.
The morphometric relations of impact craters on Mercury measured from MESSENGER data are similar to those reported previously, with crater depth, rim height, wall width, and central uplift height increasing with increasing diameter (Pike,Barnouin et al.,Talpe et al., ).
Variations in morphometry are consistent with a. Impact cratering as a geologic process on the terrestrial planets is addressed. The crater densities on the Earth and Moon form the basis for a standard flux-time curve, which can be used to date unsampled planetary surfaces and constrain the.
Our best-known example of such a large crater, Meteor Crater in Arizona (Figure ), is ab years old. However, the cratering rate can be estimated from the number of craters on the lunar maria or calculated from the number of potential “projectiles” (asteroids and comets) present in.
To gain insight into the geological processes that modified the basin morphology, we explored the distribution of MOLA MEGDR measured depths (d) and diameters (D) of impact craters in Isidis Planitia by applying known d / D power laws, representing the statistical behavior of impact crater.
crater size to mare age. • The data for this investigation were recorded at the same time as Investigations 1 and 2, using the same method of image analysis. • Instead of simply recording a gross number of craters, we recorded crater diameters as well, measured with calipers. heights. Record data and crater observations.
Set B - Drop the projectiles from different heights (suggest m). Record all height data and crater observations. 5. Discuss the effects caused by the variables. About This Activity Students do controlled cratering experiments in dry materials. They vary the impactor velocity or mass and observe.onstrated that impact cratering has been, and still is, a major process in the origin and evolution of all the solid bodies of the solar system, from Mercury to the moons of Neptune (for summaries and references, see Taylor,Chapter 3;Chapter 4).
The abundant craters on the surface of our Moon (Figs. and ) had been known for.Barringer Crater (Meteor Crater) in Arizona, United States, is a simple crater created when a meter-wide (foot-wide) iron-rich meteroid struck Earth's surface ab years ago — a very recent event to a geologist.
The crater is about kilometers (a little more than miles) across and meters ( feet) deep.