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DMAAC – February 1973
LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base. -
Lunar Sourcebook : a User's Guide to the Moon
4 LUNAR SURFACE PROCESSES Friedrich Hörz, Richard Grieve, Grant Heiken, Paul Spudis, and Alan Binder The Moon’s surface is not affected by atmosphere, encounters with each other and with larger planets water, or life, the three major agents for altering throughout the lifetime of the solar system. These terrestrial surfaces. In addition, the lunar surface has orbital alterations are generally minor, but they not been shaped by recent geological activity, because ensure that, over geological periods, collisions with the lunar crust and mantle have been relatively cold other bodies will occur. and rigid throughout most of geological time. When such a collision happens, two outcomes are Convective internal mass transport, which dominates possible. If “target” and “projectile” are of comparable the dynamic Earth, is therefore largely absent on the size, collisional fragmentation and annihilation Moon, and so are the geological effects of such occurs, producing a large number of much smaller internal motions—volcanism, uplift, faulting, and fragments. If the target object is very large compared subduction—that both create and destroy surfaces on to the projectile, it behaves as an “infinite halfspace,” Earth. The great contrast between the ancient, stable and the result is an impact crater in the target body. Moon and the active, dynamic Earth is most clearly For collisions in the asteroid belt, many of the shown by the ages of their surfaces. Nearly 80% of the resulting collisional fragments or crater ejecta escape entire solid surface of Earth is <200 m.y. old. In the gravitational field of the impacted object; many of contrast, >99% of the lunar surface formed more than these fragments are then further perturbed into 3 b.y. -
A New View on the Solar Wind Interaction with the Moon
Bhardwaj et al. Geosci. Lett. (2015) 2:10 DOI 10.1186/s40562-015-0027-y REVIEW Open Access A new view on the solar wind interaction with the Moon Anil Bhardwaj1* , M B Dhanya1, Abhinaw Alok1, Stas Barabash2, Martin Wieser2, Yoshifumi Futaana2, Peter Wurz3, Audrey Vorburger4, Mats Holmström2, Charles Lue2, Yuki Harada5 and Kazushi Asamura6 Abstract Characterised by a surface bound exosphere and localised crustal magnetic fields, the Moon was considered as a passive object when solar wind interacts with it. However, the neutral particle and plasma measurements around the Moon by recent dedicated lunar missions, such as Chandrayaan-1, Kaguya, Chang’E-1, LRO, and ARTEMIS, as well as IBEX have revealed a variety of phenomena around the Moon which results from the interaction with solar wind, such as backscattering of solar wind protons as energetic neutral atoms (ENA) from lunar surface, sputtering of atoms from the lunar surface, formation of a “mini-magnetosphere” around lunar magnetic anomaly regions, as well as several plasma populations around the Moon, including solar wind protons scattered from the lunar surface, from the mag- netic anomalies, pick-up ions, protons in lunar wake and more. This paper provides a review of these recent findings and presents the interaction of solar wind with the Moon in a new perspective. Keywords: Moon, Solar wind, ENAs, Plasma, Mini-magnetosphere, Lunar wake, Pickup ions, SARA, CENA, SWIM, Chandrayaan-1, Kaguya, Chang’E-1, ARTEMIS, IBEX Introduction charge state and ≤28 % as hydrogen energetic neutral The Moon is a regolith covered planetary object char- atoms (ENAs), existence of “mini-magnetosphere” at the acterised by a surface-bound exosphere (Killen and Ip lunar surface, reflection of solar wind protons from lunar 1999; Stern 1999; Sridharan et al. -
19910005721.Pdf
ii- ...... .. _TT i _- ..... n ,i, i ii .,_ - "-r ii .J- i ii1[11 , .... --- 77'' i - II"-- -.-- ........ ._ . ;m ... _- . ;;7.. --___'7- ,r, .... ,f_...]!,.i.,_ ......... ... ._..... NASA Technical Memorandum 4221 A Bibliography of Planetary Geology and Geophysics Principal Investigators and Their Associates, 1989-1990 NASA Office of Space Science and Applications Washington, D. C. NI A National Aeronautics and Space Administration Office of Management Scientific and Technical Information Division 1990 Contents Asteroids, Comets, and Meteorites 3 Outer Planets, Satellites, and Rings 5 Photogrammetry, Geodesy, and Cartography 7 Geologic Mapping, Stratigraphy, and Geomorphology 9 Structure and Tectonics 14 Volcanic Processes and Landforms 18 Aeolian Studies 23 Fluvial Processes 25 Impact Cratering Processes 27 Planetary Interiors and Petrology 30 Geochemistry: Regolith, Volatiles, and Atmospheres 32 Remote Sensing 34 Spectroscopy 35 Photometry 39 Radar 4O Planetary Dynamics and Cosmogony 43 General Interest Topics 46 Author Index 47 iii i'_._/__ ..... _rENTm_JI 1 PRECEDING PAGE BLANK NOT FILMED A Bibliography of Planetary Geology and Geophysics Principal Investigators and Their Associates, 1989-1990 This document is a compilation of selected bibliographic data specifically relating to recent publications submitted by principal investigators and their associates, supported through NASA's Office of Space Science and Applications, Solar System Exploration Division, Planetary Geology and Geophysics Program, and serves as a companion piece to NASA TM-4210, Reports of Planetary Geology and Geophysics Program--1989, NASA, Washington, D.C. 20546. Asteroids, Comets, and Meteorites Bell, J.F., Davis, D.R., Hartmann, W.K., and Gaffey, MJ. (1989) Asteroids: The Big Picture. In Asteroids II, ed. -
User Guide To
USER GUIDE TO 1 2 5 0 , 000 S CA L E L U NA R MA P S DANNY C. KINSLER Lunar Science Institute 3303 NASA Road #1 Houston, TX 77058 Telephone: 713/488-5200 Cable Address: LUNSI The Lunar Science Institute is operated by the Universities Space Research Association under Contract No. NSR 09-051-001 with the National Aeronautics and Space Administration. This document constitutes LSI Contribution No. 206 March 1975 USER GUIDE TO 1 : 250 , 000 SCALE LUNAR MAPS GENERAL In 1 972 the NASA Lunar Programs Office initiated the Apoll o Photographic Data Analysis Program. The principal point of this program was a detail ed scientific analysis of the orbital and surface experiments data derived from Apollo missions 15, 16, and 17 . One of the requirements of this program was the production of detailed photo base maps at a useabl e scale . NASA in conjunction with the Defense Mapping Agency (DMA) commenced a mapping program in early 1973 that would lead to the production of the necessary maps based on the need for certain areas . This paper is desi gned to present in outline form the neces- sary background information for users to become familiar with the program. MAP FORMAT The scale chosen for the project was 1:250,000* . The re- search being done required a scale that Principal Investigators (PI's) using orbital photography could use, but would also serve PI's doing surface photographic investigations. Each map sheet covers an area four degrees north/south by five degrees east/west. The base is compiled from vertical Metric photography from Apollo missions 15, 16, and 17. -
Accepted Manuscript
Accepted Manuscript Explosive volcanism on Mercury: analysis of vent and deposit morphology and modes of eruption Lauren M. Jozwiak , James W. Head , Lionel Wilson PII: S0019-1035(17)30191-4 DOI: 10.1016/j.icarus.2017.11.011 Reference: YICAR 12695 To appear in: Icarus Received date: 1 March 2017 Revised date: 31 October 2017 Accepted date: 6 November 2017 Please cite this article as: Lauren M. Jozwiak , James W. Head , Lionel Wilson , Explosive volcanism on Mercury: analysis of vent and deposit morphology and modes of eruption, Icarus (2017), doi: 10.1016/j.icarus.2017.11.011 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. ACCEPTED MANUSCRIPT 1 Highlights: Explosive volcanic morphologies on Mercury are divided into three classes. We present analysis of vent dimensions, locations, and stratigraphic ages. We find evidence for formation into relatively recent mercurian history. We use vent morphology and location to determine formation geometry. We find support for eruptions both at and above critical gas volume fractions. ACCEPTED MANUSCRIPT ACCEPTED MANUSCRIPT 2 Explosive volcanism on Mercury: analysis of vent and deposit morphology and modes of eruption Lauren M. Jozwiak1,2*, James W. Head1 and Lionel Wilson1,3 1Department of Earth, Environmental and Planetary Sciences, Brown University, 324 Brook Street Box 1846, Providence, RI, 02912 2*Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA. -
Farside-Nearside Solar Wind Precipitation Asymmetry
Planetary and Space Science xxx (2018) 1–14 Contents lists available at ScienceDirect Planetary and Space Science journal homepage: www.elsevier.com/locate/pss Space weathering on the Moon: Farside-nearside solar wind precipitation asymmetry E. Kallio a,*, S. Dyadechkin b, P. Wurz c, M. Khodachenko b,d a Electronics and Nanoengineering, School of Electrical Engineering, Aalto University, Espoo, Finland b Space Research Institute, Austrian Academy of Sciences, Graz, A-8042, Austria c Physikalisches Institut, University of Bern, Switzerland d Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia ABSTRACT The lunar surface is continuously under the impact of solar wind plasma, which breaks the chemical bonds of the surface material resulting in weathering of the surface and a modified chemical composition. Ion impact also sputters the surface material, affecting the composition of the lunar exosphere, and it controls the electrical properties of both the lunar surface and the near surface space. We have studied the lunar farside-nearside (FN) hemispherical asymmetry of the solar wind proton impact on the lunar surface along the orbit of the Moon during fast solar wind conditions. The analysis is based on a 3D hybrid model where ions are accelerated by the macroscopic j  B and pressure gradient forces. The derived proton impact surface map shows that the highest cumulative solar wind proton addition on the lunar surface is located on the farside while the most energetic protons precipitate on the nearside. The total ion impact rate was found to be smallest when the Moon is deep in the magnetotail. The total ion impact rate on the lunar surface varies while the Moon orbits the Earth and these longitudinal variations are caused by the magnetosphere and lunar tidal locking. -
Trans-Neptunian Space and the Post-Pluto Paradigm
Trans-Neptunian Space and the Post-Pluto Paradigm Alex H. Parker Department of Space Studies Southwest Research Institute Boulder, CO 80302 The Pluto system is an archetype for the multitude of icy dwarf planets and accompanying satellite systems that populate the vast volume of the solar system beyond Neptune. New Horizons’ exploration of Pluto and its five moons gave us a glimpse into the range of properties that their kin may host. Furthermore, the surfaces of Pluto and Charon record eons of bombardment by small trans-Neptunian objects, and by treating them as witness plates we can infer a few key properties of the trans-Neptunian population at sizes far below current direct-detection limits. This chapter summarizes what we have learned from the Pluto system about the origins and properties of the trans-Neptunian populations, the processes that have acted upon those members over the age of the solar system, and the processes likely to remain active today. Included in this summary is an inference of the properties of the size distribution of small trans-Neptunian objects and estimates on the fraction of binary systems present at small sizes. Further, this chapter compares the extant properties of the satellites of trans-Neptunian dwarf planets and their implications for the processes of satellite formation and the early evolution of planetesimals in the outer solar system. Finally, this chapter concludes with a discussion of near-term theoretical, observational, and laboratory efforts that can further ground our understanding of the Pluto system and how its properties can guide future exploration of trans-Neptunian space. -
History of the Lunar Orbiter Program April 1977 Performing Organization Code 6
( REPRODUCED BY U.S. DEPARTMENT OF COMMERCE NATIONAL TECHNICAL INFORMATION SERVICE SPRINGFIELD, VA 22161 ' Report No. Government Accession No. Recipient's Catalog No. 1. -�2. 3. NASA TM X-3487 Title and Subtitle 5. !WPOrt Date 4. DESTINATION MOON: A History of the Lunar Orbiter Program April 1977 Performing Organization Code 6. ADA Author(s) Performing Organization Report No. 7. 8. TMX 3487 Bruce K. Byers Work Unit No. 10. Performing Organization Name and Address not applicable 9. History Office National Aeronautics and Space Administration Contract or Grant No. 11. Headquarters not applicable Washington D.C. Type of Report and Period Covered 13. 12. Sponsoring Agency Name and Address NATIONAL AERONAUTICS 3PACE ADMINISTRATION HISTORY 1963 - 1970 Sponsoring Agency Code WASHINGTON, D.C. AND 20546 14. ADA 15. Supplementary Notes Abstract 16. This publication documents the origins of the Lunar Orbiter Program and records the activities of the missions then in progress. Covers the period when Lunar Orbiters were providing the Apollo program with photographic and selenodetic 1963data -for 1970 evaluating proposed astronaut landing sites ORIG PA INAL GE IS OF POOR QUALITY Key Words (Suggested by Author(s)) Distribution Statement 17. Apollo landing site selection 18. In addition to normal computerized Lunar exploration, unmanned, far-side; distribution, lOO copies to history radiation dosages, micrometeoriod flux, office, Code ADA and Oopies to Langley dual image, photography, image enhancement Research Center (J. Marshall300 Hughes ) . convergent stereoscopic photography Mascons, Moon's gravitational field Cat. 12 Security aassif. (of this report) Security Classif. (of this page) 21. No. of Pages Price• 19. 20. 22. -
The Moon 35 Years After Apollo: What's Left to Learn?
ARTICLE IN PRESS Chemie der Erde ] (]]]]) ]]]–]]] www.elsevier.de/chemer INVITED REVIEW The Moon 35 years after Apollo: What’s left to learn? Clive R. Nealà Chair of the Lunar Exploration Analysis Group (LEAG), Department of Civil Engineering and Geological Sciences, University of Notre Dame, Notre Dame, IN 46556, USA Received 11 December 2007; accepted 29 July 2008 Abstract With the cancellation of the Apollo program after Apollo 17 returned from the Moon in 1972, the focus of NASA switched to other areas of the Solar System. Study of the Moon did continue through analysis of the returned samples and remotely sensed data sets (both orbital and surface), as well as through Earth-based telescopic studies. In the 1990s, new orbital data were obtained from several missions (fly-by and orbital), the first being Galileo that allowed the lunar farside to be mapped, followed by global mapping by the Clementine and Lunar Prospector missions. Interest in the Moon started to increase at the beginning of the 21st century as other nations focused their space exploration programs on the Moon. The speech by President Bush in January 2004 put the Moon back into the critical exploration path for NASA, paving the way for humans to return to the lunar surface by 2020. This return will be critical for developing technologies and protocols for the eventual human exploration of other parts of the solar system. At the time of writing (June 2008), the SELENE/Kaguya mission (Japan and Chang’e-1 (China) are orbiting the Moon, with Chandrayaan-1 (India) and Lunar Reconnaissance Orbiter (USA) being scheduled to launch later in 2008. -
Measurement and Analysis of Lunar Basin Depths from Clementine Altimetry
ICARUS 131, 107±122 (1998) ARTICLE NO. IS975856 Measurement and Analysis of Lunar Basin Depths from Clementine Altimetry Kevin K. Williams1 Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, Maryland 21218 E-mail: [email protected] and Maria T. Zuber Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139-4307; and Laboratory for Terrestrial Physics, NASA/Goddard Space Flight Center, Greenbelt, Maryland Received April 3, 1997; revised August 22, 1997 Moon's early evolution (Safronov 1972, Kaula 1979). The Altimetric pro®les from the Clementine LIDAR are used to geometries and subsurface structures of large impact basins calculate the depths of 29 large craters and basins on the Moon. preserve a record of the mechanics of impact, the nature Plotting the depths of the best preserved structures together of basin modi®cation, and the thermal and physical proper- with values for simple and complex craters measured in pre- ties of the early Moon. Until recently, the geometries of Clementine studies reveals an in¯ection in the depth/diameter major basins could not be studied in detail in a collective (d/D) curve in addition to the one revealed by pre-Clementine sense because uniform, high quality topographic coverage data. This in¯ection occurs in the diameter range that corres- did not exist. Recently, the Clementine mission (Nozette ponds to the morphologic transition from complex crater to et al. et al. basin. The best empirical power law ®t for basin depths is 1994) provided near-global topography (Zuber 0.57 1994, Smith et al.