Published 1976
by Lunar Science Institute in Houston .
Written in English
Edition Notes
Includes bibliographical references and indexes.
| Statement | compiled by the Lunar Science Institute. |
| Series | LSI contribution ;, 259 |
| Contributions | Lunar Science Institute., Geological Survey (U.S.). Branch of Astrogeologic Studies. |
| Classifications | |
|---|---|
| LC Classifications | QB581 .L76 no. 259, QB603.C7 .L76 no. 259 |
| The Physical Object | |
| Pagination | ix, 169 p. : |
| Number of Pages | 169 |
| ID Numbers | |
| Open Library | OL4915611M |
| LC Control Number | 76150334 |
the effect of a planet's atmosphere upon the cratering process in the present paper and refer readers to [Melosh, Chapt. XI; O'Keefe and Ahrens, ; Roddy et al.f ; Schultz and Gault, ]. To calculate the impact-induced flow fields within the solid planets, we used the Eulerian-Lagrangian code developed by Thompson []. The key. papers presented to the symposium on planetary cratering mechanics lunar science institute topical conference hosted by the u. s. geological survey, geologic division branch of astrogeologic studies flagstaff, arizona september compiled by the lunar science institute nasa road 1 houston, texas i lsi contribution universitatsbibuothek hannover technische. Our approach was to numerically compute the evolution of impact induced flow fields and calculate the time histories of the key measures of crater geometry (e.g. depth, diameter, lip height) for variations in planetary gravity (0 to 10 9 cm/s 2), material strength (0 to kbar), and impactor radius ( to km). These results were used to establish the values of the open parameters in the scaling laws Cited by: 17, O'KEEFE AND AHRENS: PLANETARY CRATERING MECHANICS TABLE 1. Scope of Parameters Studied for Impact of Silicate Projectile on a Planetary Half-Space Parameter Symbol Value Employed Unit Impact velocity Planetary gravity Density Bulk modulus U 12 g O, 1, 10 2, 4, 5, x Se r E x km/s ge ( cm/s 2) g/cm 3 dyn/cm 2.
Proceedings of the Symposium on Planetary Cratering Mechanics, Flagstaff, Ariz., September 13–17, (A78– 19–91), Pergamon Press, New York () Google ScholarCited by: 2. Abstract The objective of this study was to obtain a quantitative understanding of the cratering process over a broad range of conditions. Our approach was to numerically compute the evolution of impact induced flow fields and calculate the time histories of the key measures of crater geometry (e.g., depth, diameter, lip height) for variations in planetary gravity (0 to 10 9 cm/s 2), material. Planetary cratering mechanics. By John D. Okeefe and Thomas J. Ahrens. Abstract. To obtain a quantitative understanding of the cratering process over a broad range of conditions, we have numerically computed the evolution of impact induced flow fields and calculated the time histories of the major measures of crater geometry (e.g., depth Author: John D. Okeefe and Thomas J. Ahrens. The 6th meeting on Cosmic Dust (Cosmic Dust VI) is held at CPS (Center for Planetary Science), Kobe, Japan from Monday, August 5, through Friday, August 9, This issue of Planetary and Space Science will be primarily devoted to Cosmic Dust VI and contain the papers presented .
This volume contains papers which were accepted for publication by the Organizing Committee of the Symposium on Planetary Cratering Mechanics. Papers were solicited which addressed one of the following major topics: I. Experimental studies II. Planetary impact cratering III. Theoretical calculations IV. Scaling. Terrestrial impact structures—Principal characteristics and energy considerations. Impact and explosion cratering: Planetary and terrestrial implications. Proceedings of the Symposium on Planetary Cratering Mechanics, Flagstaff, Arizona (A ), Pergamon Press, New York, Inc. pp. – Google Scholar. prl, ahmedabad moon surface books lunar and planetary science 12 abstracts of papers submitted to the papers presented to the symposium on planetary cratering mechanics held in arizona in () lun b 37 vandehulst hc ed. Abstract. The objective of this study was to obtain a quantitative understanding of the cratering process over a broad range of conditions. Our approach was to numerically compute the evolution of impact induced flow fields and calculate the time histories of the key measures of crater geometry (e.g. depth, diameter, lip height) for variations in planetary gravity (0 to 10^9 cm/s^2), material Author: John D. O&#;Keefe and Thomas J. Ahrens.
