PPT-Empirical ejecta thickness laws for impact craters:

McGetchin Settle amp Head EPSL 20 1973 RADIAL THICKNESS VARIATION IN IMPACT CRATER EJECTA IMPLICATIONS FOR LUNAR BASIN DEPOSITS t 014R 074 rR 30 What is used here McGetchin takes R to be final crater radius not transient crater radius as erroneously indicated by Melosh. Background also see Teachers Guide Pages 1 2 photo on 8 12 and photo on 13 The circular features so obvious on the Moons surface are impact craters formed when impactors smashed into the surface The explosion and excavation of materials at the impac These impact craters have formed on the surfaces over the 46 billion year age of our solar system The number of craters on a surface increases with the length of time that surface ha s been exposed to space These rather simple ideas are the basis fo RE - - HALOED IMPACT CRATERS: NEW CRITERIA FOR MODERN DATA SETS . I. Antonenk o , 1 Planetary Institute of Toronto, 197 Fairview Ave. Toronto, ON M6P 3A6, Ca n ada (PlanetaryInstituteofToronto@yahoo Nadine G. Barlow. Dept. Physics and Astronomy. Northern Arizona University. Flagstaff, AZ 86011-6010. Nadine.Barlow@nau.edu. Office: 928-523-5452 Cell: 928-600-9253. Co-authors: Joseph M. Boyce (U. HI) and Lionel Wilson (Lancaster U.). Francis Nimmo. Last Week - Volcanism. How and why are melts generated?. Increase in mantle potential temperature; or. Reduction in solidus temperature (e.g. water); or. Thinning of the lithosphere. How do melts ascend towards the surface?. ejecta. thickness laws for impact craters:. McGetchin. , Settle & Head EPSL 20 (1973) . RADIAL THICKNESS VARIATION IN IMPACT CRATER EJECTA:. IMPLICATIONS FOR LUNAR BASIN DEPOSITS. t = 0.14R. 0.74. Characterizing LROC NAC Images. Created by: . Belfry High School. Participants. Taylor Runyon. Mickayla Walters. Sarah Compton. Staci Coleman. Brianna Sullivan. Our Purpose. Our purpose of doing this project is to understand morphology and the composition of the Tycho . Palaeomagnetic. properties of randomly. oriented basaltic blocks from Lonar crater . ejecta. , India. Md. Arif. 1. , N. Basavaiah. 1. and S. Misra. 2. 1. Indian Institute of Geomagnetism (IIG), New Panvel, . March 11, 2014. Earth 438. Rampart Craters: A Case for Water on Mars. Outline. What. What is a Rampart Crater?. Cratering Mechanics and . Types. Why. Rampart Crater Formation Theory. Where. Rampart Craters on Mars. Geoffrey George, Charles Gutierrez Miguel . Nze. , Matt Malacara, Brandon Rangel, Juan . Urquidi. , Alex Valdez. Robert E. Lee High School/S.T.E.M. RAM Academy. San Antonio, Texas. Project Selection. Una Hwang (NASA/GSFC, JHU). &. J Martin Laming (NRL). Boston AAS 24 May 2011. Cas A First-light Chandra image (Hughes+ 2000). Red: Fe. , . Green: Si . Cassiopeia A. . Core-collapse SNR with the most prominent Fe ejecta emission. Fall . 2007. 4 October . 2007. Class . #10. Review. Venus resurfacing event(s) 300-500 . Myr. ago. Just how do you determine the age of a planetary surface?. Impacts. Mars. Martian Crustal Magnetization. Doctrinal Research. : Research . in Law. . It studies the Legal Propositions . based on . Secondary Data . of authorities such as . Conventional Legal Theories. , . Laws. , . Statutory . materials, . properties of randomly. oriented basaltic blocks from Lonar crater . ejecta. , India. Md. Arif. 1. , N. Basavaiah. 1. and S. Misra. 2. 1. Indian Institute of Geomagnetism (IIG), New Panvel, . Navi.