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Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km. -
Sa Abá, ¡Ay! ¡Chito! Ó ¡Chiton!. Sht...! ¡Chiton! ¡Silencio!
English_Spanish_Tagalog_Dictionary_Project_Gutenberg_cd3wd !Vaya! ¡que vergüenza!. Ayan! kahiyâhiyâ! ¡Ah! ¡ay!. Ah! abá! ahá! ¡Ay!. Sa abá, ¡ay! ¡Chito! ó ¡chiton!. Sht...! ¡Chiton! ¡silencio!. ¡Marahan! ¡Fuera! ¡fuera de aquí! ¡quita! ¡quita allá!. Sulong! tabì! lumayas ka! alis diyan! ¡He! ¡oye!. Hoy! pakinggan mo! ¡He!. Ehé. ¡Oh!. Abá! ¡Quita de ahí! ¡vete allá!. Tabì! sulong! ¡Vaya!. ¡Ayan! A bordo. Nakasakay sa sasakyán. A cada hora. Oras-oras. Á cada momento. Sa bawa't sangdalî. A Dios. Paalam, adyos. A Dios; despedida. Paalam. Á él mismo. Sa kanya ngâ, sa kanya man, sa kanya rin (lalake). Á eso, á ello. Diyan sa, doon sa. Á eso, á ello. Diyan sa, doon sa. A este ó esta, por eso. Dahil dito. A esto. Dito sa; hanggang dito. A esto. Dito sa, hanggang dito. Á horcajadas. Pahalang. A la mar, fuera del navio. Sa tubig. A la moda. Ayon sa ugalí, sunod sa moda. A la temperatura de la sangre. Kasing-init ng dugô. Á lo ancho. Sa kalwangan. Á lo cual. Dahil dito, sa dahilang ito. A lo largo. Sa gawî, sa hinabahabà. Á lo largo. Sa hinabahabà. Á lo que, á que. Na saan man. Á mas, ademas. Bukod sa rito, sakâ. A medio camino. Sa may kalagitnaan ng lakarín. Á menos que; si no. Maliban, kung dî. A pedacitos. Tadtad. Á pie. Lakád. A poca distancia, cercanamente. Malapítlapít, halos. Spanish_Tagalog Page 1 English_Spanish_Tagalog_Dictionary_Project_Gutenberg_cd3wd Á poco precio. May kamurahan. A popa, en popa. Sa gawíng likod, sa gawíng hulí. A popa. Sa gawíng likod. Á propósito. Bagay. A punto de, dispuesto á, en accion. Kauntî na, handâ na, hala. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Durham Research Online
Durham Research Online Deposited in DRO: 02 June 2020 Version of attached le: Accepted Version Peer-review status of attached le: Peer-reviewed Citation for published item: Heap, Michael J. and Gilg, H. Albert and Byrne, Paul K. and Wadsworth, Fabian B. and Reuschl¡e,Thierry (2020) 'Petrophysical properties, mechanical behaviour, and failure modes of impact melt-bearing breccia (suevite) from the Ries impact crater (Germany).', Icarus., 349 . p. 113873. Further information on publisher's website: https://doi.org/10.1016/j.icarus.2020.113873 Publisher's copyright statement: c 2020 This manuscript version is made available under the CC-BY-NC-ND 4.0 license http://creativecommons.org/licenses/by-nc-nd/4.0/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full DRO policy for further details. Durham University Library, Stockton Road, Durham DH1 3LY, United Kingdom Tel : +44 (0)191 334 3042 | Fax : +44 (0)191 334 2971 https://dro.dur.ac.uk Journal Pre-proof Petrophysical properties, mechanical behaviour, and failure modes of impact melt-bearing breccia (suevite) from the Ries impact crater (Germany) Michael J. -
Large Impact Crater Histories of Mars: the Effect of Different Model Crater Age Techniques ⇑ Stuart J
Icarus 225 (2013) 173–184 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Large impact crater histories of Mars: The effect of different model crater age techniques ⇑ Stuart J. Robbins a, , Brian M. Hynek a,b, Robert J. Lillis c, William F. Bottke d a Laboratory for Atmospheric and Space Physics, 3665 Discovery Drive, University of Colorado, Boulder, CO 80309, United States b Department of Geological Sciences, 3665 Discovery Drive, University of Colorado, Boulder, CO 80309, United States c UC Berkeley Space Sciences Laboratory, 7 Gauss Way, Berkeley, CA 94720, United States d Southwest Research Institute and NASA Lunar Science Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, United States article info abstract Article history: Impact events that produce large craters primarily occurred early in the Solar System’s history because Received 25 June 2012 the largest bolides were remnants from planet ary formation .Determi ning when large impacts occurred Revised 6 February 2013 on a planetary surface such as Mars can yield clues to the flux of material in the early inner Solar System Accepted 25 March 2013 which, in turn, can constrain other planet ary processes such as the timing and magnitude of resur facing Available online 3 April 2013 and the history of the martian core dynamo. We have used a large, global planetary databas ein conjunc- tion with geomorpholog icmapping to identify craters superposed on the rims of 78 larger craters with Keywords: diameters D P 150 km on Mars, 78% of which have not been previously dated in this manner. -
El Cerebro De Broca
El cerebro de Broca es un libro escrito por Carl Sagan formado por discursos o artículos publicados entre 1974 y 1979 en muchas revistas incluyendo Atlantic Monthly, New Republic, Physics Today, Playboy, y Scientific American. El ensayo que titula el libro lleva su nombre en honor del físico, anatomista y antropólogo francés, Paul Broca (1824-1880). Generalmente se recuerda a Broca por su descubrimiento de que distintas partes físicas del cerebro corresponden a distintas funciones. Una gran parte del libro está dedicada a desacreditar el trabajo de los «fabricantes de paradojas», como llama a los divulgadores de la pseudociencia, ya sea quienes se encuentran al borde de las disciplinas científicas o simplemente son rotundos charlatanes. Otra gran parte del libro discute los convencionalismos en la nomenclatura de los miembros de nuestro sistema solar, así como sus características físicas. Sagan también expone sus puntos de vista sobre la Ciencia Ficción, mencionando especialmente a Robert A. Heinlein, quien fue uno de sus escritores favoritos durante su infancia. Las experiencias cercanas a la muerte, y sus controversias culturales también son discutidas en el libro, así como la crítica de las teorías desarrolladas en el libro de Robert K. Temple The Sirius Mystery publicado tres años antes en 1975. Carl Sagan El cerebro de Broca ePub r1.3 Horus 05.08.16 Título original: Broca´s Brain Carl Sagan, 1974, 1975, 1976, 1977, 1978, 1979 Traducción: Doménech Bregada (Cap 1 al 7) y José Chabás (Cap 8 al 25) Diseño de portada: Horus Editor digital: Horus Colaborador: epubsagan (apéndices y tablas) Corrección de erratas: el nota, heutorez, Autillo ePub base r1.2 Para Rachel y Samuel Sagan, mis padres, que introdujeron en mí la alegría de la comprensión del mundo, con gratitud, admiración y amor AGRADECIMIENTOS EN CUANTO A DISCUSIÓN de puntos específicos abordados en el texto, estoy en deuda con un buen número de amigos, corresponsales y colegas, entre los que se incluyen Diane Ackerman, D.W.G. -
Constraints on Mechanisms for the Growth of Gully Alcoves in Gasa Crater, Mars, from Two-Dimensional Stability Assessments of Rock Slopes ⇑ Chris H
Icarus 211 (2011) 207–221 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Constraints on mechanisms for the growth of gully alcoves in Gasa crater, Mars, from two-dimensional stability assessments of rock slopes ⇑ Chris H. Okubo a, , Livio L. Tornabene b, Nina L. Lanza c a Astrogeology Science Center, U.S. Geological Survey, Flagstaff, AZ 86001, United States b Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, United States c Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, United States article info abstract Article history: The value of slope stability analyses for gaining insight into the geologic conditions that would facilitate Received 6 December 2009 the growth of gully alcoves on Mars is demonstrated in Gasa crater. Two-dimensional limit equilibrium Revised 29 September 2010 methods are used in conjunction with high-resolution topography derived from stereo High Resolution Accepted 30 September 2010 Imaging Science Experiment (HiRISE) imagery. These analyses reveal three conditions that may produce Available online 27 November 2010 observed alcove morphologies through slope failure: (1) a ca. >10 m thick surface layer that is either sat- urated with H2O ground ice or contains no groundwater/ice at all, above a zone of melting H2O ice or Keywords: groundwater and under dynamic loading (i.e., seismicity), (2) a 1–10 m thick surface layer that is satu- Mars, Surface rated with either melting H O ice or groundwater and under dynamic loading, or (3) a >100 m thick sur- Geological processes 2 Tectonics face layer that is saturated with either melting H2O ice or groundwater and under static loading. -
Pectatqk AUGUST 13, 2009 * a PIONEER PRESS PUBLICATION * * $2.00 THIS WEEK
NILES t1G'43 2009 tise PECTATQk AUGUST 13, 2009 * A PIONEER PRESS PUBLICATION * WWW.PIONEERLOCALCOM * $2.00 THIS WEEK Dl VERSIONS Nile. Public Library Dietrict 6960 Oakton Street Nile., IllInois 60714 (847) 663-1234 DROP iN ANYTIME The romance "The Time-Traveler's a' Wife" is featured in this week's Film Clips. SEE PAGEB2 FOOD FUEL UP! New Wilmette cooking school just for kids. SEE PIONEERLOCALCOM 0 s- p' Bradley Augustyn, 11, hits a beach ball into the air with friends Aug. 4 at the Nues Police D, HANG TIME Department's National Night Out event at St. John Brebeuf Church. PAGE 5. (Allison Williams/Staff Photographer) Start here withahealth care career. ii s1It4 Attend a free Health Care information Session. t'4D.L)O'3I1Ítd 1S1IH 39 .I.$IO Health Information echnology .Lsra,.tjtJJ8I1 3i'1l1dS1IN Monday, August 17, at 1 p.m., Des Plaines Campus, Room 2846 O_DL01 For more information, call 847.635.1957. Oakton 1600 East Golf Road, Des Plaineswww.oakton.edu ?Community College z www.pioneerlocal.com THURSDAY, AUGUST 13. 2009 CONTAcT: Matt Schmitz, Assistant Managing Editor IPAGE 3 p: 708.524.4433 e:[email protected] SWANCC Document The new'y designedbairdwarner.com destruction Real estat&s best web site is'roweven better. Superior content, unsurpassed TEEN IDOL property details, and a user experience that's highly Savannah Koziol, 13, of event to be d'namic and just plain easier. Aurora, sings "Our Song" Saturday at the Aug. 22 Teen Idol singingcoto- Did somebody say "Wow?" petition at Golf Mill Oh yeah, you did. -
XV Congresso Nazionale Di Scienze Planetarie PRESIDENTE DEL CONGRESSO: Giovanni Pratesi
https://doi.org/10.3301/ABSGI.2019.01 Firenze, 4-8 Febbraio 2019 ABSTRACT BOOK a cura della Società Geologica Italiana XV Congresso Nazionale di Scienze Planetarie PRESIDENTE DEL CONGRESSO: Giovanni Pratesi. COMITATO SCIENTIFICO: Giovanni Pratesi, Emanuele Pace, Marco Benvenuti, John Brucato, Fabrizio Capaccioni, Sandro Conticelli, Aldo Dell’Oro, Carlo Alberto Garzonio, Daniele Gardiol, Monica Lazzarin, Alessandro Marconi, Lucia Mari- nangeli, Giuseppina Micela, Ettore Perozzi, Alessandro Rossi, Alessandra Rotundi. COMITATO ORGANIZZATORE: Cristian Carli, Mario Di Martino, Livia Giacomini, Vanni Moggi Cecchi, Emanuele Pace, Giovanni Pratesi, Giovanni Valsecchi. CURATORI DEL VOLUME Giovanni Pratesi, Fabrizio Capaccioni, Emanuele Pace, John Brucato, Marco Benvenuti, Sandro Conti- celli, Aldo Dell’Oro, Daniele Gardiol, Carlo Alberto Garzonio, Monica Lazzarin, Alessandro Marconi, Lucia Marinangeli, Giuseppina Micela, Ettore Perozzi, Alessandro Rossi, Alessandra Rotundi. Papers, data, figures, maps and any other material published are covered by the copyright own by the Società Geologica Italiana. DISCLAIMER: The Società Geologica Italiana, the Editors are not responsible for the ideas, opinions, and contents of the papers published; the authors of each paper are responsible for the ideas opinions and con- tents published. La Società Geologica Italiana, i curatori scientifici non sono responsabili delle opinioni espresse e delle affermazioni pubblicate negli articoli: l’autore/i è/sono il/i solo/i responsabile/i. ABSTRACT INDEX EDUCARE ALLA -
Nr 05/2016 Mycket Plats För Studenterna
[s 26] Porträttet: Jutta Haider bland fåglar och foliehattar [s 4] I höst lär UR oss att SVENSK BIBLIOTEKFÖRENINGS programmera med barnen TIDNING UTGIVEN SEDAN 1916 [s 23] Ny modell: Dubbelt så nr 05/2016 mycket plats för studenterna BBL 1001916–2016 Plats för ALLA [s 12] Ingen visste vad Garaget skulle fyllas med. Nu är det fullt med folk. FÖR INNE ORD HÅLL I nummer 5 2016 2 LEDARE 4 JUST NU 9 MÅNADENS ELIN 10 TEMA: BYGG DIN EGEN BY Är det någon 12 Garaget i Malmö 16 Så fyller du biblioteket Sidenblus mot en FOTO: JOHANNA WALLIN JOHANNA FOTO: 17 Nya verktyg mäter bredden bomullsscarf? Nora 18 Bildning sker lokalt s 12 och hennes mamma 20 Fullt program i Queens fyndar på Garagets Lundaforskaren Jutta Haider som vill ha mig? studerar vad nätets algoritmer klädbytardag i Malmö. s 26 låter oss få veta – och varför. år reporter Sofia Wixner satt besökarna i fokus och öppnat för det som 22 DET VAR DÅ lånar i det här numret ut sig rör sig i lokalsamhället. Ur mitt 23 NY MODELL: KTHB själv till en biblioteksbesö- Några av frågorna i det här temat väcktes bibliotek kare i aktiviteten ”Låna en under en lunch med Axiells seniorkonsult Boris 26 INTERVJU: JUTTA HAIDER Språket, obönhörlig- svensk” på biblioteket i Falun. Ukotic Zetterlund – av hans ivrigt viftande heten, sinnligheten 30 DEBATT Hon formulerar med möda händer medan han berättade om hur bibliote- och ondskan sätter en lapp som ska locka en av ken med en ny matematik kan gasa istället för Sofi Oksanens 32 SÅ GJORDE VI: DET MAGISKA ORDET Faluns biblioteksbesökare att bromsa. -
O Lunar and Planetary Institute Provided by the NASA Astrophysics Data System ANCIENT MARTIAN CRATERED TERRAIN MATERIALS EXPOSED by DEFLATION N.W
ANCIENT MARTIAN CRATERED TERRAIN MATERIALS EXPOSED BY DEFLATION NORTHWEST OF THE BALDET AND ANTONIADI BASINS; R. Arvidson, E. Guinness, C. Leff, M. Presl ey, Dept. of Earth and Planetary Sci . , Washington Univ. , St. Louis, Mo. 63130 and R. Saunders, L. Rothy Jet Propulsion Laboratory, Pasadena, Ca. 911 09 In 1979 some 2400 Viking Orbiter images were acquired in the northern cratered terrains of Mars, between Chryse Planitia and Isidis Planitia (Albee et al., 1980). The data provide contiguous coverage over a strip approximately 350km wide in a N-S direction and 6500km wide in an E-W direc- tion. The spatial resolution varies from 15 to 60 meters per pixel. These data provide both the high resolution needed to identify surface processes that have operated within the cratered terrains, and the synoptic coverage needed to determine the areal extent and importance of the processes. As the starting point of an interdisciplinary examination of the morphology, color, a1 bedo, thermal , and radar properties of the northern cratered terrains we have characterized the landforms and processes evident in the cratered terrains to the north and northwest of the basins Baldet and Antoniadi (see Orbiter mosaics 21 1-5936 to 5939). The cratered terrain centered at approximately 25' N. lat, 295' W. long, is distinctly different in appearance than the cratered terrain several hun- dred kilometers to the west. The western area exhibits smooth intercrater plains supporting a population of craters that appears to be in production. Numerous clusters of well preserved secondary craters can also be seen. Toward the east, north of Baldet and Antoniadi, the cratered terrain has been dissected into a series of elongate plateaus and ridges.