A Three Year Report 2009-2012
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LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned
Space Sci Rev DOI 10.1007/s11214-011-9759-y LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned Jennifer L. Heldmann · Anthony Colaprete · Diane H. Wooden · Robert F. Ackermann · David D. Acton · Peter R. Backus · Vanessa Bailey · Jesse G. Ball · William C. Barott · Samantha K. Blair · Marc W. Buie · Shawn Callahan · Nancy J. Chanover · Young-Jun Choi · Al Conrad · Dolores M. Coulson · Kirk B. Crawford · Russell DeHart · Imke de Pater · Michael Disanti · James R. Forster · Reiko Furusho · Tetsuharu Fuse · Tom Geballe · J. Duane Gibson · David Goldstein · Stephen A. Gregory · David J. Gutierrez · Ryan T. Hamilton · Taiga Hamura · David E. Harker · Gerry R. Harp · Junichi Haruyama · Morag Hastie · Yutaka Hayano · Phillip Hinz · Peng K. Hong · Steven P. James · Toshihiko Kadono · Hideyo Kawakita · Michael S. Kelley · Daryl L. Kim · Kosuke Kurosawa · Duk-Hang Lee · Michael Long · Paul G. Lucey · Keith Marach · Anthony C. Matulonis · Richard M. McDermid · Russet McMillan · Charles Miller · Hong-Kyu Moon · Ryosuke Nakamura · Hirotomo Noda · Natsuko Okamura · Lawrence Ong · Dallan Porter · Jeffery J. Puschell · John T. Rayner · J. Jedadiah Rembold · Katherine C. Roth · Richard J. Rudy · Ray W. Russell · Eileen V. Ryan · William H. Ryan · Tomohiko Sekiguchi · Yasuhito Sekine · Mark A. Skinner · Mitsuru Sôma · Andrew W. Stephens · Alex Storrs · Robert M. Suggs · Seiji Sugita · Eon-Chang Sung · Naruhisa Takatoh · Jill C. Tarter · Scott M. Taylor · Hiroshi Terada · Chadwick J. Trujillo · Vidhya Vaitheeswaran · Faith Vilas · Brian D. Walls · Jun-ihi Watanabe · William J. Welch · Charles E. Woodward · Hong-Suh Yim · Eliot F. Young Received: 9 October 2010 / Accepted: 8 February 2011 © The Author(s) 2011. -
Small, Young Volcanic Deposits Around the Lunar Farside Craters Rosseland, Bolyai, and Roche
44th Lunar and Planetary Science Conference (2013) 2024.pdf SMALL, YOUNG VOLCANIC DEPOSITS AROUND THE LUNAR FARSIDE CRATERS ROSSELAND, BOLYAI, AND ROCHE. J. H. Pasckert1, H. Hiesinger1, and C. H. van der Bogert1. 1Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany. jhpasckert@uni- muenster.de Introduction: To understand the thermal evolu- mare basalts on the near- and farside. This gives us the tion of the Moon it is essential to investigate the vol- opportunity to investigate the history of small scale canic history of both the lunar near- and farside. While volcanism on the lunar farside. the lunar nearside is dominated by mare volcanism, the farside shows only some isolated mare deposits in the large craters and basins, like the South Pole-Aitken basin or Tsiolkovsky crater [e.g., 1-4]. This big differ- ence in volcanic activity between the near- and farside is of crucial importance for understanding the volcanic evolution of the Moon. The extensive mare volcanism of the lunar nearside has already been studied in great detail by numerous authors [e.g., 4-8] on the basis of Lunar Orbiter and Apollo data. New high-resolution data obtained by the Lunar Reconnaissance Orbiter (LRO) and the SELENE Terrain Camera (TC) now allow us to investigate the lunar farside in great detail. Basaltic volcanism of the lunar nearside was active for almost 3 Ga, lasting from ~3.9-4.0 Ga to ~1.2 Ga before present [5]. In contrast to the nearside, most eruptions of mare deposits on the lunar farside stopped much earlier, ~3.0 Ga ago [9]. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Relative Ages
CONTENTS Page Introduction ...................................................... 123 Stratigraphic nomenclature ........................................ 123 Superpositions ................................................... 125 Mare-crater relations .......................................... 125 Crater-crater relations .......................................... 127 Basin-crater relations .......................................... 127 Mapping conventions .......................................... 127 Crater dating .................................................... 129 General principles ............................................. 129 Size-frequency relations ........................................ 129 Morphology of large craters .................................... 129 Morphology of small craters, by Newell J. Fask .................. 131 D, method .................................................... 133 Summary ........................................................ 133 table 7.1). The first three of these sequences, which are older than INTRODUCTION the visible mare materials, are also dominated internally by the The goals of both terrestrial and lunar stratigraphy are to inte- deposits of basins. The fourth (youngest) sequence consists of mare grate geologic units into a stratigraphic column applicable over the and crater materials. This chapter explains the general methods of whole planet and to calibrate this column with absolute ages. The stratigraphic analysis that are employed in the next six chapters first step in reconstructing -
PDF Program Book
46th Meeting of the Division for Planetary Sciences with Historical Astronomy Division (HAD) 9-14 November 2014 | Tucson, AZ OFFICERS AND MEMBERS ........ 2 SPONSORS ............................... 2 EXHIBITORS .............................. 3 FLOOR PLANS ........................... 5 ATTENDEE SERVICES ................. 8 Session Numbering Key SCHEDULE AT-A-GLANCE ........ 10 100s Monday 200s Tuesday SUNDAY ................................. 20 300s Wednesday 400s Thursday MONDAY ................................ 23 500s Friday TUESDAY ................................ 44 Sessions are numbered in the program book by day and time. WEDNESDAY .......................... 75 All posters will be on display Monday - Friday THURSDAY.............................. 85 FRIDAY ................................. 119 Changes after 1 October are included only in the online program materials. AUTHORS INDEX .................. 137 1 DPS OFFICERS AND MEMBERS Current DPS Officers Heidi Hammel Chair Bonnie Buratti Vice-Chair Athena Coustenis Secretary Andrew Rivkin Treasurer Nick Schneider Education and Public Outreach Officer Vishnu Reddy Press Officer Current DPS Committee Members Rosaly Lopes Term Expires November 2014 Robert Pappalardo Term Expires November 2014 Ralph McNutt Term Expires November 2014 Ross Beyer Term Expires November 2015 Paul Withers Term Expires November 2015 Julie Castillo-Rogez Term Expires October 2016 Jani Radebaugh Term Expires October 2016 SPONSORS 2 EXHIBITORS Platinum Exhibitor Silver Exhibitors 3 EXHIBIT BOOTH ASSIGNMENTS 206 Applied -
Branches Vol 22
Branches volume wen y- wo Caldwell Community College and Technical Institute 2855 Hickory Boulevard Hudson, North Carolina 28638 828.726.2200 • 828.297.3811 www.cccti.edu CCC TI is an equal opportunity educator employer Cindy Meissner Untitled Relief Print Acknowledgements Art Editors Laura Aultman Justin Butler Thomas Thielemann Literary Editors Heather Barnett Jessica Chapman DeAnna Chester Brad Prestwood Production Director Ron Wilson Special Thanks: Alison Beard Ron Holste Martin Moore Edward Terry Linda Watts Funding and other support for Branches was provided by the CCC&TI Foundation, the College Transfer Division and the Department of Fine Arts, umanities, Social Sciences, and Physical Education. To view previous editions of Branches or to find out more information about submitting works of art or literature to the 23rd edition of Branches, please visit our website at www.cccti.edu/branches. Table of Contents Factory Reflection ......................................Scott Garnes ................................Frontispiece Sunday Afternoon with Flamenco ..............KJ Maj ..........................................................1 Woman on the Liffey Bridge........................Peter Morris ..................................................3 Void ............................................................Katie Webb....................................................4 Yellow ospital Garments ..........................Mattea Richardson ........................................5 Canned Peaches in Winter ..........................Amy -
Binary Asteroids and the Formation of Doublet Craters
ICARUS 124, 372±391 (1996) ARTICLE NO. 0215 Binary Asteroids and the Formation of Doublet Craters WILLIAM F. BOTTKE,JR. Division of Geological and Planetary Sciences, California Institute of Technology, Mail Code 170-25, Pasadena, California 91125 E-mail: [email protected] AND H. JAY MELOSH Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona 85721 Received April 29, 1996; revised August 14, 1996 found we could duplicate the observed fraction of doublet cra- At least 10% (3 out of 28) of the largest known impact craters ters found on Earth, Venus, and Mars. Our results suggest on Earth and a similar fraction of all impact structures on that any search for asteroid satellites should place emphasis Venus are doublets (i.e., have a companion crater nearby), on km-sized Earth-crossing asteroids with short-rotation formed by the nearly simultaneous impact of objects of compa- periods. 1996 Academic Press, Inc. rable size. Mars also has doublet craters, though the fraction found there is smaller (2%). These craters are too large and too far separated to have been formed by the tidal disruption 1. INTRODUCTION of an asteroid prior to impact, or from asteroid fragments dispersed by aerodynamic forces during entry. We propose that Two commonly held paradigms about asteroids and some fast rotating rubble-pile asteroids (e.g., 4769 Castalia), comets are that (a) they are composed of non-fragmented after experiencing a close approach with a planet, undergo tidal chunks of rock or rock/ice mixtures, and (b) they are soli- breakup and split into multiple co-orbiting fragments. -
Apollo Over the Moon: a View from Orbit (Nasa Sp-362)
chl APOLLO OVER THE MOON: A VIEW FROM ORBIT (NASA SP-362) Chapter 1 - Introduction Harold Masursky, Farouk El-Baz, Frederick J. Doyle, and Leon J. Kosofsky [For a high resolution picture- click here] Objectives [1] Photography of the lunar surface was considered an important goal of the Apollo program by the National Aeronautics and Space Administration. The important objectives of Apollo photography were (1) to gather data pertaining to the topography and specific landmarks along the approach paths to the early Apollo landing sites; (2) to obtain high-resolution photographs of the landing sites and surrounding areas to plan lunar surface exploration, and to provide a basis for extrapolating the concentrated observations at the landing sites to nearby areas; and (3) to obtain photographs suitable for regional studies of the lunar geologic environment and the processes that act upon it. Through study of the photographs and all other arrays of information gathered by the Apollo and earlier lunar programs, we may develop an understanding of the evolution of the lunar crust. In this introductory chapter we describe how the Apollo photographic systems were selected and used; how the photographic mission plans were formulated and conducted; how part of the great mass of data is being analyzed and published; and, finally, we describe some of the scientific results. Historically most lunar atlases have used photointerpretive techniques to discuss the possible origins of the Moon's crust and its surface features. The ideas presented in this volume also rely on photointerpretation. However, many ideas are substantiated or expanded by information obtained from the huge arrays of supporting data gathered by Earth-based and orbital sensors, from experiments deployed on the lunar surface, and from studies made of the returned samples. -
Southwestern M O N U M E N
SOUTHWESTERN MONUMENTS MONTHLY REPORT OCTOBER - - - - 1938 DEPARTMENT OF THE INTERIOR NATIONAL PARK SERVICE SOUTHWESTERN MONUMENTS OCTOBER, 1338, REPORT INDEX OPENING, by Superintendent Frank Pinkley, 27,1 CONDENSED GENERAL REPORT Travel ........... ,277 400 Flora, Fauna, and Natural 000 General. -278 Fhenomena. .280 100 Administrative . , . .278 500 Tse of Facilities by Public,280 200 Maintenance, Improvements, 600 Protection 281 and New Construction . .279 700 Archeology, Fist. ,Pre-Hist... 281 300 Activities Other .Agencies,279 900 Miscellaneous. ...... 282 RETORTS FPOM KEN IN THE FIE'D Arches .£34 Gran Ouivi'-a. ......... .294 Aztec Ruins ......... -.284 Hove:.weep 286 Bandelier .... ...... ..297 Mobile Unit .......... .336 Bandelier CCC ..... .299 Montezuma Jastle. ........ ,305 Bandelier Forestry. , .300 Natural Fridges ........ .320 Canyon de Chelly. ...... .318 • Navajo .312 Capulin Mountain. ...... ,319 pipe Spring 292 Casa Grande .......... -308 Saguaro ............ .237 Casa Grande Side Camp .... .310 Sunset Crater ......... .291 Chaco Canyon. ........ .302 Tumacacori. .......... .312 Chiricahua. ......... .295 -Yalnut Canyon ......... .301 Chiricahua CCC. ....... .296 White Sands .......... .283 El Morrc. .......... .315 Wupatki 289 HEADQUARTERS Aztec Ruins Visitor Statistics.333 Casa Grande Visitor Statistics. .331 Branch of Accounting. .... .339 Comparative Visitor Figures . .329 Branch of Education ..... .324 October Visitors to S.W.M 334 Branch of Maintenance .... :323 Personnel Notes 340 THE SUPPLEMENT Beaver Habitat at Bandelier, By W. B. McDcugall ..... .351 Geology Notes on the Montezuma Castle Region, by E..C. Alberts. .353 Geology Report on the Hovenweep National Monument, by C. N. Gould . .357 Moisture Retention of Cacti,'by David J.'Jones 353 Ruminations, by The Boss. '.'•'. .361 Supplemental Observations, from the- Field ........ .344 , SOUTHWESTERN MONUMENTS PERSONNEL HEADQUARTERS: National Park Service, Coolidge, Arizona. Frank Pinkley, Superintendent; Hugh M. -
•- 61 GEORGE C, T/B ' 5( 5-O< /. , B
https://ntrs.nasa.gov/search.jsp?R=19650015410 2020-03-24T05:08:03+00:00Z •- 61 MDWG-63-2 April I, 1963 GEORGE C, A BIBLIOGRAPHY CONCERNING ASPECTS OF THE METEOROID HAZARD by The MSFC Meteoroid Damage Working Group GPO PRICE $ = 11 (THRU) / OTS PRICElS) $ (PA ESJ (CODE) I _A6A_R OR "rMx OR _.D NUMmlERI (CATEGORy) Hard copy (HC)_ T/b_' 5(_ 5-o< Microfiche (MF) /. _,_b MSFC . Form 454 ('Revlzed September 1961) I rJ_r MDWG-63-2 April i, 1963 A BIBLIOGRAPHY CONCERNING ASPECTS OF THE METEOROID HAZARD by The MSFC Meteoroid Damage Working Group John B. Gayle Engineering Materials Branch Propulsion & Vehicle Engineering Division, Chairman Charles C. Dalton Aerophysics & Astrophysics Branch, Aeroballistics Division Henry L. Martin Physics & Astrophysics Branch, Research Projects Division William D. Murphree Assistant to Director, Aeroballistics Division Charlotte F. Shenk Redstone Scientific Information Center (ex officio) Army Missile Command GEORGE C. MARSHALL SPACE FLIGHT CENTER Huntsville, Alabama FOREWORD This bibliography, consisting of 876 entries, was compiled to present information on the physics of hypervelocity impact and the meteoroid hazard. Divided into nine general sections, it contains Surveys of Experimental Data, Vehicle Protection Analysis, Theoretical Studies (Hypervelocity Impact), Experimental Investigations, Experi- ments and Instrumentation, and Theoretical Studies (Meteoritics). An author index for Part A begins on page 143; the author index for Part B begins on page 283. Most of the references are fairly recent, having been published between January 1950 and October 1962. The entries were obtained from all knownsources, and the author, title, agency, periodical, and ASTIAnumbers (whenknown) are included. -
Roche Limit. Formation of Small Aggregates
ROYAL OBSERVATORY OF BELGIUM On the formation of the Martian moons from a circum-Mars accretion disk Rosenblatt P. and Charnoz S. 46th ESLAB Symposium: Formation and evolution of moons Session 2 – Mechanism of formation: Moons of terrestrial planets June 26th 2012 – ESTEC, Noordwijk, the Netherlands. The origin of the Martian moons ? Deimos (Viking image) Phobos (Viking image)Phobos (MEX/HRSC image) Size: 7.5km x 6.1km x 5.2km Size: 13.0km x 11.39km x 9.07km Unlike the Moon of the Earth, the origin of Phobos & Deimos is still an open issue. Capture or in-situ ? 1. Arguments for in-situ formation of Phobos & Deimos • Near-equatorial, near-circular orbits around Mars ( formation from a circum-Mars accretion disk) • Mars Express flybys of Phobos • Surface composition: phyllosilicates (Giuranna et al. 2011) => body may have formed in-situ (close to Mars’ orbit) • Low density => high porosity (Andert, Rosenblatt et al., 2010) => consistent with gravitational-aggregates 2. A scenario of in-situ formation of Phobos and Deimos from an accretion disk Adapted from Craddock R.A., Icarus (2011) Giant impact Accretion disk on Proto-Mars Mass: ~1018-1019 kg Gravitational instabilities formed moonlets Moonlets fall Two moonlets back onto Mars survived 4 Gy later elongated craters Physical modelling never been done. What modern theories of accretion can tell us about that scenario? 3. Purpose of this work: Origin of Phobos & Deimos consistent with theories of accretion? Modern theories of accretion : 2 main regimes of accretion. • (a) The strong tide regime => close to the planet ~ Roche Limit Background : Accretion of Saturn’s small moons (Charnoz et al., 2010) Accretion of the Earth’s moon (Canup 2004, Kokubo et al., 2000) • (b) The weak tide regime => farther from the planet Background : Accretion of big satellites of Jupiter & Saturn Accretion of planetary embryos (Lissauer 1987, Kokubo 2007, and works from G. -
Survivability of Copper Projectiles During Hypervelocity Impacts in Porous
Icarus 268 (2016) 102–117 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Survivability of copper projectiles during hypervelocity impacts in porous ice: A laboratory investigation of the survivability of projectiles impacting comets or other bodies ⇑ K.H. McDermott, M.C. Price, M. Cole, M.J. Burchell Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NH, United Kingdom article info abstract Article history: During hypervelocity impact (>a few km sÀ1) the resulting cratering and/or disruption of the target body Received 27 October 2014 often outweighs interest on the outcome of the projectile material, with the majority of projectiles Revised 4 December 2015 assumed to be vaporised. However, on Earth, fragments, often metallic, have been recovered from impact Accepted 11 December 2015 sites, meaning that metallic projectile fragments may survive a hypervelocity impact and still exist Available online 6 January 2016 within the wall, floor and/or ejecta of the impact crater post-impact. The discovery of the remnant impac- tor composition within the craters of asteroids, planets and comets could provide further information Keywords: regarding the impact history of a body. Accordingly, we study in the laboratory the survivability of 1 Impact processes and 2 mm diameter copper projectiles fired onto ice at speeds between 1.00 and 7.05 km sÀ1. The projec- Cratering À1 Mars tile was recovered intact at speeds up to 1.50 km s , with no ductile deformation, but some surface pit- À1 Meteorites ting was observed. At 2.39 km s , the projectile showed increasing ductile deformation and broke into À1 Comet Tempel-1 two parts.