Map Area] Crest of Prominent Wrinkle Ridges (Fig
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Minutes of the January 25, 2010, Meeting of the Board of Regents
MINUTES OF THE JANUARY 25, 2010, MEETING OF THE BOARD OF REGENTS ATTENDANCE This scheduled meeting of the Board of Regents was held on Monday, January 25, 2010, in the Regents’ Room of the Smithsonian Institution Castle. The meeting included morning, afternoon, and executive sessions. Board Chair Patricia Q. Stonesifer called the meeting to order at 8:31 a.m. Also present were: The Chief Justice 1 Sam Johnson 4 John W. McCarter Jr. Christopher J. Dodd Shirley Ann Jackson David M. Rubenstein France Córdova 2 Robert P. Kogod Roger W. Sant Phillip Frost 3 Doris Matsui Alan G. Spoon 1 Paul Neely, Smithsonian National Board Chair David Silfen, Regents’ Investment Committee Chair 2 Vice President Joseph R. Biden, Senators Thad Cochran and Patrick J. Leahy, and Representative Xavier Becerra were unable to attend the meeting. Also present were: G. Wayne Clough, Secretary John Yahner, Speechwriter to the Secretary Patricia L. Bartlett, Chief of Staff to the Jeffrey P. Minear, Counselor to the Chief Justice Secretary T.A. Hawks, Assistant to Senator Cochran Amy Chen, Chief Investment Officer Colin McGinnis, Assistant to Senator Dodd Virginia B. Clark, Director of External Affairs Kevin McDonald, Assistant to Senator Leahy Barbara Feininger, Senior Writer‐Editor for the Melody Gonzales, Assistant to Congressman Office of the Regents Becerra Grace L. Jaeger, Program Officer for the Office David Heil, Assistant to Congressman Johnson of the Regents Julie Eddy, Assistant to Congresswoman Matsui Richard Kurin, Under Secretary for History, Francisco Dallmeier, Head of the National Art, and Culture Zoological Park’s Center for Conservation John K. -
Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
1922 Elizabeth T
co.rYRIG HT, 192' The Moootainetro !scot1oror,d The MOUNTAINEER VOLUME FIFTEEN Number One D EC E M BER 15, 1 9 2 2 ffiount Adams, ffiount St. Helens and the (!oat Rocks I ncoq)Ora,tecl 1913 Organized 190!i EDITORlAL ST AitF 1922 Elizabeth T. Kirk,vood, Eclttor Margaret W. Hazard, Associate Editor· Fairman B. L�e, Publication Manager Arthur L. Loveless Effie L. Chapman Subsc1·iption Price. $2.00 per year. Annual ·(onl�') Se,·ent�·-Five Cents. Published by The Mountaineers lncorJ,orated Seattle, Washington Enlerecl as second-class matter December 15, 19t0. at the Post Office . at . eattle, "\Yash., under the .-\0t of March 3. 1879. .... I MOUNT ADAMS lllobcl Furrs AND REFLEC'rION POOL .. <§rtttings from Aristibes (. Jhoutribes Author of "ll3ith the <6obs on lltount ®l!!mµus" �. • � J� �·,,. ., .. e,..:,L....._d.L.. F_,,,.... cL.. ��-_, _..__ f.. pt",- 1-� r�._ '-';a_ ..ll.-�· t'� 1- tt.. �ti.. ..._.._....L- -.L.--e-- a';. ��c..L. 41- �. C4v(, � � �·,,-- �JL.,�f w/U. J/,--«---fi:( -A- -tr·�� �, : 'JJ! -, Y .,..._, e� .,...,____,� � � t-..__., ,..._ -u..,·,- .,..,_, ;-:.. � --r J /-e,-i L,J i-.,( '"'; 1..........,.- e..r- ,';z__ /-t.-.--,r� ;.,-.,.....__ � � ..-...,.,-<. ,.,.f--· :tL. ��- ''F.....- ,',L � .,.__ � 'f- f-� --"- ��7 � �. � �;')'... f ><- -a.c__ c/ � r v-f'.fl,'7'71.. I /!,,-e..-,K-// ,l...,"4/YL... t:l,._ c.J.� J..,_-...A 'f ',y-r/� �- lL.. ��•-/IC,/ ,V l j I '/ ;· , CONTENTS i Page Greetings .......................................................................tlristicles }!}, Phoiitricles ........ r The Mount Adams, Mount St. Helens, and the Goat Rocks Outing .......................................... B1/.ith Page Bennett 9 1 Selected References from Preceding Mount Adams and Mount St. -
Origin of Circular Collapsed Landforms in the Chryse Region of Mars ⇑ Manuel Roda A,B, , Maarten G
Icarus 265 (2016) 70–78 Contents lists available at ScienceDirect Icarus journal homepage: www.journals.elsevier.com/icarus Origin of circular collapsed landforms in the Chryse region of Mars ⇑ Manuel Roda a,b, , Maarten G. Kleinhans b, Tanja E. Zegers b, Rob Govers b a Universitá degli Studi di Milano, Dipartimento di Scienze della Terra, Via Mangiagalli, 34, 20133 Milano, Italy b Universiteit Utrecht, Faculty of Geosciences, Heidelberglaan 2, 3584 CS Utrecht, The Netherlands article info abstract Article history: The quasi-circular collapsed landforms occurring in the Chryse region of Mars share similar morpholog- Received 29 June 2015 ical characteristics, such as depth of collapse and polygonally fractured floors. Here, we present a statis- Revised 20 October 2015 tical analysis of diameter, maximum and minimum depth, and amount of collapse of these features. Accepted 21 October 2015 Based on their morphometric characteristics, we find that these landforms have a common origin. In par- Available online 27 October 2015 ticular, the investigated landforms show diameter-depth correlations similar to those that impact craters of equivalent diameters exhibit. We also find that the observed amount of collapse of the collected fea- Keywords: tures is strongly correlated to their diameter. Furthermore, the linear relation between minimum filling Geological processes and pristine depth of craters, the constant ratio between collapse and the amount of filling and the frac- Ices Impact processes tured and chaotic aspect of the filling agree with melting and subsequent collapse of an ice layer below a Mars, surface sediment layer. This interpretation is consistent with a buried sub-ice lake scenario, which is a non-climatic mechanism for producing and storing abundant liquid water under martian conditions. -
Formation of Aromatum Chaos, Mars: Morphological Development As a Result of Volcano-Ice Interactions Harald J
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, E08071, doi:10.1029/2005JE002549, 2006 Formation of Aromatum Chaos, Mars: Morphological development as a result of volcano-ice interactions Harald J. Leask,1 Lionel Wilson,1 and Karl L. Mitchell1,2 Received 3 August 2005; revised 10 May 2006; accepted 16 May 2006; published 17 August 2006. [1] Morphological examination of the Aromatum Chaos depression on Mars supports earlier suggestions that it is a site of cryosphere disruption and release of pressurized water trapped in an underlying aquifer. We infer that the cause of cryosphere disruption was intrusion of a volcanic sill, confined laterally by earlier intruded dikes, and consequent melting of ice by heat from the sill. The vertical extents and displacements of blocks of terrain on the floor of the depression, together with an estimate of the cryosphere thickness, constrain the vertical extent of ice melting and hence the thickness of the sill (100 m) and the depth at which it was intruded (2–5 km). At least 75% of the volume of material removed from Aromatum Chaos must have been crustal rock rather than melted ice. Water from melted cryosphere ice played a negligible role in creating the depression, the process being dominated by released aquifer water. For sediment loads of 30–40% by volume, 10,500–16,500 km3 of aquifer water must have passed through the depression to carry away rock as entrained sediment and erode the associated Ravi Vallis channel. These required water volumes are 2–3 times larger than the amount of water that could reasonably be contained in aquifers located beneath the area of incipiently collapsed ground to the west of Aromatum Chaos and suggest a much larger water source. -
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, -
Testing Hypotheses for the Origin of Steep Slope of Lunar Size-Frequency Distribution for Small Craters
CORE Metadata, citation and similar papers at core.ac.uk Provided by Springer - Publisher Connector Earth Planets Space, 55, 39–51, 2003 Testing hypotheses for the origin of steep slope of lunar size-frequency distribution for small craters Noriyuki Namiki1 and Chikatoshi Honda2 1Department of Earth and Planetary Sciences, Kyushu University, Hakozaki 6-10-1, Higashi-ku, Fukuoka 812-8581, Japan 2The Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara 229-8510, Japan (Received June 13, 2001; Revised June 24, 2002; Accepted January 6, 2003) The crater size-frequency distribution of lunar maria is characterized by the change in slope of the population between 0.3 and 4 km in crater diameter. The origin of the steep segment in the distribution is not well understood. Nonetheless, craters smaller than a few km in diameter are widely used to estimate the crater retention age for areas so small that the number of larger craters is statistically insufficient. Future missions to the moon, which will obtain high resolution images, will provide a new, large data set of small craters. Thus it is important to review current hypotheses for their distributions before future missions are launched. We examine previous and new arguments and data bearing on the admixture of endogenic and secondary craters, horizontal heterogeneity of the substratum, and the size-frequency distribution of the primary production function. The endogenic crater and heterogeneous substratum hypotheses are seen to have little evidence in their favor, and can be eliminated. The primary production hypothesis fails to explain a wide variation of the size-frequency distribution of Apollo panoramic photographs. -
Identification of Volcanic Rootless Cones, Ice Mounds, and Impact 3 Craters on Earth and Mars: Using Spatial Distribution As a Remote 4 Sensing Tool
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 111, XXXXXX, doi:10.1029/2005JE002510, 2006 Click Here for Full Article 2 Identification of volcanic rootless cones, ice mounds, and impact 3 craters on Earth and Mars: Using spatial distribution as a remote 4 sensing tool 1 1 1 2 3 5 B. C. Bruno, S. A. Fagents, C. W. Hamilton, D. M. Burr, and S. M. Baloga 6 Received 16 June 2005; revised 29 March 2006; accepted 10 April 2006; published XX Month 2006. 7 [1] This study aims to quantify the spatial distribution of terrestrial volcanic rootless 8 cones and ice mounds for the purpose of identifying analogous Martian features. Using a 9 nearest neighbor (NN) methodology, we use the statistics R (ratio of the mean NN distance 10 to that expected from a random distribution) and c (a measure of departure from 11 randomness). We interpret R as a measure of clustering and as a diagnostic for 12 discriminating feature types. All terrestrial groups of rootless cones and ice mounds are 13 clustered (R: 0.51–0.94) relative to a random distribution. Applying this same 14 methodology to Martian feature fields of unknown origin similarly yields R of 0.57–0.93, 15 indicating that their spatial distributions are consistent with both ice mound or rootless 16 cone origins, but not impact craters. Each Martian impact crater group has R 1.00 (i.e., 17 the craters are spaced at least as far apart as expected at random). Similar degrees of 18 clustering preclude discrimination between rootless cones and ice mounds based solely on 19 R values. -
Episodic Flood Inundations of the Northern Plains of Mars
www.elsevier.com/locate/icarus Episodic flood inundations of the northern plains of Mars Alberto G. Fairén,a,b,∗ James M. Dohm,c Victor R. Baker,c,d Miguel A. de Pablo,b,e Javier Ruiz,f Justin C. Ferris,g and Robert C. Anderson h a CBM, CSIC-Universidad Autónoma de Madrid, 28049 Cantoblanco, Madrid, Spain b Seminar on Planetary Sciences, Universidad Complutense de Madrid, 28040 Madrid, Spain c Department of Hydrology and Water Resources, University of Arizona, Tucson, AZ 85721, USA d Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA e ESCET, Universidad Rey Juan Carlos, 28933 Móstoles, Madrid, Spain f Departamento de Geodinámica, Universidad Complutense de Madrid, 28040 Madrid, Spain g US Geological Survey, Denver, CO 80225, USA h Jet Propulsion Laboratory, Pasadena, CA 91109, USA Received 19 December 2002; revised 20 March 2003 Abstract Throughout the recorded history of Mars, liquid water has distinctly shaped its landscape, including the prominent circum-Chryse and the northwestern slope valleys outflow channel systems, and the extremely flat northern plains topography at the distal reaches of these outflow channel systems. Paleotopographic reconstructions of the Tharsis magmatic complex reveal the existence of an Europe-sized Noachian drainage basin and subsequent aquifer system in eastern Tharsis. This basin is proposed to have sourced outburst floodwaters that sculpted the outflow channels, and ponded to form various hypothesized oceans, seas, and lakes episodically through time. These floodwaters decreased in volume with time due to inadequate groundwater recharge of the Tharsis aquifer system. Martian topography, as observed from the Mars Orbiter Laser Altimeter, corresponds well to these ancient flood inundations, including the approximated shorelines that have been proposed for the northern plains. -
A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars
minerals Review A Review of Sample Analysis at Mars-Evolved Gas Analysis Laboratory Analog Work Supporting the Presence of Perchlorates and Chlorates in Gale Crater, Mars Joanna Clark 1,* , Brad Sutter 2, P. Douglas Archer Jr. 2, Douglas Ming 3, Elizabeth Rampe 3, Amy McAdam 4, Rafael Navarro-González 5,† , Jennifer Eigenbrode 4 , Daniel Glavin 4 , Maria-Paz Zorzano 6,7 , Javier Martin-Torres 7,8, Richard Morris 3, Valerie Tu 2, S. J. Ralston 2 and Paul Mahaffy 4 1 GeoControls Systems Inc—Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA 2 Jacobs JETS Contract at NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (B.S.); [email protected] (P.D.A.J.); [email protected] (V.T.); [email protected] (S.J.R.) 3 NASA Johnson Space Center, Houston, TX 77058, USA; [email protected] (D.M.); [email protected] (E.R.); [email protected] (R.M.) 4 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA; [email protected] (A.M.); [email protected] (J.E.); [email protected] (D.G.); [email protected] (P.M.) 5 Institito de Ciencias Nucleares, Universidad Nacional Autonoma de Mexico, Mexico City 04510, Mexico; [email protected] 6 Centro de Astrobiología (INTA-CSIC), Torrejon de Ardoz, 28850 Madrid, Spain; [email protected] 7 Department of Planetary Sciences, School of Geosciences, University of Aberdeen, Aberdeen AB24 3FX, UK; [email protected] 8 Instituto Andaluz de Ciencias de la Tierra (CSIC-UGR), Armilla, 18100 Granada, Spain Citation: Clark, J.; Sutter, B.; Archer, * Correspondence: [email protected] P.D., Jr.; Ming, D.; Rampe, E.; † Deceased 28 January 2021. -
Timing of Fluvial Activity in the Xanthe Terra Region of Mars: Implications for Hypanis Delta, a Potential Landing Site for Mars2020
47th Lunar and Planetary Science Conference (2016) 2196.pdf TIMING OF FLUVIAL ACTIVITY IN THE XANTHE TERRA REGION OF MARS: IMPLICATIONS FOR HYPANIS DELTA, A POTENTIAL LANDING SITE FOR MARS2020. S. Eckes1, N.H. Warner1, S. Gup- ta2, M. O’Shea1, J. Smith1, A. Werynski1, 1Department of Geological Sciences, SUNY Geneseo, 1 College Circle, Geneseo, NY 14454; 2Imperial College London, South Kensington Campus, Earth Science and Engineering, Lon- don, SW7 2AZ, UK. [email protected] & [email protected] Introduction: The Xanthe Terra region of Mars > 200 m diameter craters rest solely on top of these exhibits multiple fluvial networks that are of interest ejecta blankets. It is possible, given the thickness of the for future exploration. The timing of these channels is ejecta blankets for (order of) 10 km-size craters and poorly constrained and it’s not clear whether they given depth/diameter relationships of craters of this formed at the same time or spanned a broader period of size [6,7], that some craters may poke through the ejec- history [1,2,3]. Furthermore, sedimentary fans that are ta from the highland terrain beneath. This scenario sourced by some of the channels are currently under would provide an overestimate of the formation age of consideration as landing sites for Mars2020. It is there- the larger crater using crater statistics. fore critical to understand their timing within the To better understand and resolve this issue, we chronostratigraphic context of Mars. Current estimates, constrained a mean thickness for each ejecta blanket in based on crater counts from the fans, places the fluvial our count analysis using a 100 m High Resolution Ste- activity within the Hesperian to Early Amazonian reo Camera digital elevation model (DEM). -
THE MOON PRE-LAB Using Your Lecture Textbook And/Or Any Other Acceptable Source of Information, Answer Each Question in Complete Sentences
Name: Date: THE MOON PRE-LAB Using your lecture textbook and/or any other acceptable source of information, answer each question in complete sentences. Be sure to define any relevant terms. 1. Explain the following terms relating to lunar surface features. a. Maria (singular “Mare”): b. Highlands: c. Rille: d. Wrinkle Ridge: e. Rays: 2. Explain the following terms relating to processes that shape the lunar surface. a. Tectonic: b. Volcanic: c. Impact: d. Dating by Superposition: 8–1 Name: Partners: Date: THE MOON LAB EXERCISE LUNAR REGIONS In completing this lab, you will view images found on the Astronomy lab website. Your instructor will direct you to the location. The Earth, the Moon and the Sun are the most familiar astronomical objects in the sky. Of these, the Moon has been historically the most studied and most photographed by astronomers. Even a small telescope reveals an incredible profusion of lunar features. The most prominent are the lunar maria, which show as dark smooth areas surrounded by mountains. Almost all of the maria are on the earthside of the Moon and have lower elevation than the lighter highlands. The worksheet is a sketch of the Moon, the meandering lines outline maria and highlands. 1. Examine the images of the near and far sides of the moon on the website. Describe the similari- ties and differences. 2. Look carefully at the image of the near side of the Moon and the map of the moon on your table. Place M’s on the worksheet at the center of the major maria.