PPT-Impact crater on Mercury (

Caloris Basin Credit NASAMessenger Barringer Meteor Crater in northern Arizona near Winslow is nearly ¾ miles across and is 570 ft deep It was created 50000 years ago by an NickelIron meteorite 50 yards across and traveling approx 30000 mihr. 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 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. Phobos. – The Age of . Phobos. and its Largest Crater Stickney. 1. N. Schmedemann. 1. , . G. Michael. 1. ,. B. A. Ivanov. 2. , . J. Murray. 3. and G. Neukum. 1. ,. . 1. Institute of Geological Sciences, . 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, . 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. palaeoregolith. deposits as sources of information about history of the Solar System. Sinitsyn M.P. . Lunar and planetary investigations division . Sternberg Astronomical Institute. Moscow State University. Int At the base of a few, mostly south-facing crater slopes in mid-southern latitudes tongue-like concave depressions with sharp, elevated bound-ing ridges extend a short distance onto the crater Phobos. C. omparison of two Endmember Chronologies. The Age and Cratering History of . Phobos. , Sept 21 2015. Outline. Background:. dating of planetary surfaces from measurements of crater size-frequency distributions. An independent discovery of subglacial impact crater in northwest Greenland by gravity aspects from Earth gravity model EIGEN 6C4 and magnetic anomaly . datad. G. Kletetschka . 1,2,3 . , , J. . Klokočník. 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. Rebecca J. Thomas*, Dave A. Rothery, Susan J. Conway, Mahesh . Anand. The Open University, U.K.. European Planetary Science Congress 2015. 2. NASA/JHUAPL/CIW, NASA/Caltech. Explosive volcanism & impact structures. McGetchin. , Settle & Head EPSL 20 (1973) . RADIAL THICKNESS VARIATION IN IMPACT CRATER EJECTA:. IMPLICATIONS FOR LUNAR BASIN DEPOSITS. t = 0.14R. 0.74. . (r/R). -3.0. . What is used here. McGetchin takes R to be final crater radius, not “transient crater radius” as erroneously indicated by Melosh.. Resource Person. ISRO - Dr. A S . Arya. Team Members. Dr. G . Sreenivasan. , RRSC-C/NRSC. Dr. . Abhik. . Kundu. , . Asutosh. College. Dr. . Phani. . Rajasekhar. , SAC. Mr. . Dhrupesh. Shah, SAC. Mr. .