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Aitken Basin
Geological and geochemical analysis of units in the South Pole – Aitken Basin A.M. Borst¹,², F.S. Bexkens¹,², B. H. Foing², D. Koschny² ¹ Department of Petrology, VU University Amsterdam ² SCI-S. Research and Scientific Support Department, ESA – ESTEC Student Planetary Workshop 10-10-2008 ESA/ESTEC The Netherlands The South Pole – Aitken Basin Largest and oldest Lunar impact basin - Diameter > 2500 km - Depth > 12 km - Age 4.2 - 3.9 Ga Formed during Late heavy bombardment? Window into the interior and evolution of the Moon Priority target for future sample return missions Digital Elevation Model from Clementine altimetry data. Produced in ENVI, 50x vertical exaggeration, orthographic projection centered on the far side. Red +10 km, purple/black -10km. (A.M.Borst et.al. 2008) 1 The Moon and the SPA Basin Geochemistry Iron map South Pole – Aitken Basin mafic anomaly • High Fe, Th, Ti and Mg abundances • Excavation of mafic deep crustal / upper mantle material Thorium map Clementine 750 nm albedo map from USGS From Paul Lucey, J. Geophys. Res., 2000 Map-a-Planet What can we learn from the SPA Basin? • Large impacts; Implications and processes • Volcanism; Origin, age and difference with near side mare basalts • Cratering record; Age, frequency and size distribution • Late Heavy Bombardment; Intensity, duration and origin • Composition of the deeper crust and possibly upper mantle 2 Topics of SPA Basin study 1) Global structure of the basin (F.S. Bexkens et al, 2008) • Rims, rings, ejecta distribution, subsequent craters modifications, reconstructive -
Submission Completed
Your abstract submission has been received Print this page You have submitted the following abstract to GSA Annual Meeting in Denver, Colorado, USA - 2016. Receipt of this notice does not guarantee that your submission was complete or free of errors. PLUTO IS THE NEW MARS! MOORE, Jeffrey M.1, MCKINNON, William B.2, SPENCER, John R.3, HOWARD, Alan D.4, GRUNDY, William M.5, STERN, S. Alan3, WEAVER, Harold A.6, YOUNG, Leslie A.3, ENNICO, Kimberly1 and OLKIN, Cathy3, (1)NASA Ames Research Center, Space Science Division, MS-245-3, Moffett Field, CA 95129, (2)Washington University, Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, One Brookings Drive, Saint Louis, MO 63130, (3)Southwest Research Institute, Boulder, CO 80302, (4)Department of Environmental Sciences, Univerisity of Virginia, PO Box 400123, Charlottesville, VA 22904-4123, (5)Lowell Observatory, Flagstaff, AZ 86001, (6)Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, [email protected] Data from NASA’s New Horizons encounter with Pluto in July 2015 revealed an astoundingly complex world. The surface seen on the encounter hemisphere ranged in age from ancient to recent. A vast craterless plain of slowly convecting solid nitrogen resides in a deep primordial impact basin, reminiscent of young enigmatic deposits in Mars’ Hellas basin. Like Mars, regions of Pluto are dominated by valleys, though the Pluto valleys are thought to be carved by nitrogen glaciers. Pluto has fretted terrain and halo craters. Pluto is cut by tectonics of several different ages. Like Mars, vast tracts on Pluto are mantled by dust and volatiles. -
New Horizons Pluto/KBO Mission Impact Hazard
New Horizons Pluto/KBO Mission Impact Hazard Hal Weaver NH Project Scientist The Johns Hopkins University Applied Physics Laboratory Outline • Background on New Horizons mission • Description of Impact Hazard problem • Impact Hazard mitigation – Hubble Space Telescope plays a key role New Horizons: To Pluto and Beyond The Initial Reconnaissance of The Solar System’s “Third Zone” KBOs Pluto-Charon Jupiter System 2016-2020 July 2015 Feb-March 2007 Launch Jan 2006 PI: Alan Stern (SwRI) PM: JHU Applied Physics Lab New Horizons is NASA’s first New Frontiers Mission Frontier of Planetary Science Explore a whole new region of the Solar System we didn’t even know existed until the 1990s Pluto is no longer an outlier! Pluto System is prototype of KBOs New Horizons gives the first close-up view of these newly discovered worlds New Horizons Now (overhead view) NH Spacecraft & Instruments 2.1 meters Science Team: PI: Alan Stern Fran Bagenal Rick Binzel Bonnie Buratti Andy Cheng Dale Cruikshank Randy Gladstone Will Grundy Dave Hinson Mihaly Horanyi Don Jennings Ivan Linscott Jeff Moore Dave McComas Bill McKinnon Ralph McNutt Scott Murchie Cathy Olkin Carolyn Porco Harold Reitsema Dennis Reuter Dave Slater John Spencer Darrell Strobel Mike Summers Len Tyler Hal Weaver Leslie Young Pluto System Science Goals Specified by NASA or Added by New Horizons New Horizons Resolution on Pluto (Simulations of MVIC context imaging vs LORRI high-resolution "noodles”) 0.1 km/pix The Best We Can Do Now 0.6 km/pix HST/ACS-PC: 540 km/pix New Horizons Science Status • -
New Horizons: Reconnaissance of the Pluto-Charon System and The
C.T. Russell Editor New Horizons Reconnaissance of the Pluto-Charon System and the Kuiper Belt Previously published in Space Science Reviews Volume 140, Issues 1–4, 2008 C.T. Russell Institute of Geophysics & Planetary Physics University of California Los Angeles, CA, USA Cover illustration: NASA’s New Horizons spacecraft was launched on 2006 January 19, received a grav- ity assist during a close approach to Jupiter on 2007 February 28, and is now headed for a flyby with closest approach 12,500 km from the center of Pluto on 2015 July 14. This artist’s depiction shows the spacecraft shortly after passing above Pluto’s highly variegated surface, which may have black-streaked surface deposits produced from cryogenic geyser activity, and just before passing into Pluto’s shadow when solar and earth occultation experiments will probe Pluto’s tenuous, and possibly hazy, atmosphere. Sunlit crescents of Pluto’s moons Charon, Nix, and Hydra are visible in the background. After flying through the Pluto system, the New Horizons spacecraft could be re-targeted towards other Kuiper Belt Objects in an extended mission phase. This image is based on an original painting by Dan Durda. © Dan Durda 2001 All rights reserved. Back cover illustration: The New Horizons spacecraft was launched aboard an Atlas 551 rocket from the NASA Kennedy Space Center on 2008 January 19 at 19:00 UT. Library of Congress Control Number: 2008944238 DOI: 10.1007/978-0-387-89518-5 ISBN-978-0-387-89517-8 e-ISBN-978-0-387-89518-5 Printed on acid-free paper. -
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, -
New Horizons Ultima Thule Flyby Events
New Horizons Ultima Thule Flyby Events – Dec 31, 2018 – Jan 3, 2019 Event Date/Time Communications Event Speaker 31 Dec 12:00 PM K‐Center Opens at Noon Guest Ops team 1:00 Welcome Adrian Hill and VIP Welcome 1:05 The New Horizons Mission Alan Stern 1:25 What is the Kuiper Belt and what are Kuiper Belt Hal Weaver Objects 1:30 What We Know About MU69 – Ultima Thule Cathy Olkin 1:35 The Flyby of MU69 – Ultima Thule John Spencer NYE press 2:00 – 3:00 Daily media update on Webcast Mike Buckley; panel: Alan Stern, Helene Winters, John Spencer, Fred Pelletier. 3:15 ‐ 3:45 Flyby Ask Me Anything Webcast Moderator Adrian Hill; Panelists: Kelsi Singer; Alex Parker; Gabe Rogers 3:45 – 3:50 Song ‐ Acoustic Craig Werth – move to dining area 3:50 ‐ 4:45 Exploration for Kids Janet Ivey of Janet’s Planet ‐ dining area 4:45‐4:50 Closeout Afternoon 5:00 Doors Close for 2 hours – dinner break 7:00 PM K center reopens Kick off. 8:00 Welcome Adrian Hill and VIPs 8:10 Solar System Archaeology Ken Lacovara 8:15 NASA’s Study of Ancient Bodies. Small bodies mission panel. OSIRIS‐REx (Barnouin), Lucy (Levison), Psyche (Elkins), NH (Stern) *NASA Rep 9:00 Short break Transition to Guest ops. 9:15 Craig Werth Video Craig Werth 9:20 Doing Geology by Looking Up; Doing Walter Alvarez Astronomy by Looking Down 9:35 Pluto Flyby: Summer of 2015 Hal Weaver 9:50 Pluto and the Human Imagination David Grinspoon 10:10 Break 10:20 Meet the New Horizons Team Alan Stern and Helene Winters 10:30 Finding MU69 – Ultima Thule Marc Buie 10:45 MU69: What we expect to learn Panel: Silvia Protopapa, Hal Weaver, Cathy Olkin, John Spencer 11:00 The Eyes and Ears of New Horizons Kelsi Singer, Kirby Runyon. -
New Horizons SOC to Instrument Pipeline ICD
New Horizons SOC to Instrument Pipeline ICD September 2017 SwRI® Project 05310 Document No. 05310-SOCINST-01 Contract NASW-02008 Prepared by SOUTHWEST RESEARCH INSTITUTE® Space Science and Engineering Division 6220 Culebra Road, San Antonio, Texas 78228-0510 (210) 684-5111 FAX (210) 647-4325 Southwest Research Institute 05310-SOCINST-01 Rev 0 Chg 0 New Horizons SOC to Instrument Pipeline ICD Page ii New Horizons SOC to Instrument Pipeline ICD SwRI Project 05310 Document No. 05310-SOCINST-01 Contract NASW-02008 Prepared by: Joe Peterson 08 November 2013 Revised by: Brian Carcich August, 2014 Revised by: Tiffany Finley March, 2016 Revised by: Tiffany Finley October, 2016 Revised by: Brian Carcich December, 2016 Revised by: Tiffany Finley, Brian Carcich, PEPSSI team April, 2017 Revised by: Tiffany Finley, PEPSSI team September, 2017 Contributors: ALICE specifics prepared by: Maarten Versteeg, Joel Parker, & Andrew Steffl LEISA specifics prepared by: George McCabe & Allen Lunsford LORRI specifics prepared by: Hal Weaver & Howard Taylor MVIC specifics prepared by: Cathy Olkin PEPSSI specifics prepared by: Stefano Livi, Matthew Hill, Lawrence Brown, & Peter Kollman REX specifics prepared by: Ivan Linscott & Brian Carcich SDC specifics prepared by: David James SWAP specifics prepared by: Heather Elliott Southwest Research Institute 05310-SOCINST-01 Rev 0 Chg 0 New Horizons SOC to Instrument Pipeline ICD Page iii General Approval Signatures: Approved by: ____________________________________ Date: ____________ Hal Weaver, JHU/APL, Project Scientist -
Slope - Geologic Age Relationships in Complex Lunar Craters C
49th Lunar and Planetary Science Conference 2018 (LPI Contrib. No. 2083) 2399.pdf SLOPE - GEOLOGIC AGE RELATIONSHIPS IN COMPLEX LUNAR CRATERS C. Rojas1, P. Mahanti1, M. S. Robinson1, LROC Team1, 1LROC Science Operation Center, School of Earth and Space Exploration, Arizona State University, Tempe, Arizona ([email protected]) Table 1: List of complex craters. *Copernican craters Introduction: Impact events leading to formation Crater D (km) Model Age (Ga) Lon Lat of basins and large craters dominate the early history Moore F* 24 0.041∓0.012 [8] 37.30 185.0 of the Moon [1] leading to kilometer scale topographic Wiener F* 30 0.017∓0.002 149.9740.90 variations on the lunar surface, with smaller crater [2], Klute W* 31 0.090∓0.007 216.7037.98 progressively introducing higher frequency topography. Necho* 37 0.080∓0.024 [8] 123.3 –5.3 Crater wall slopes represent most of the overall topo- Aristarchus* 40 0.175∓0.0095 312.5 23.7 graphic variation since many locations on the Moon are Jackson* 71 0.147∓0.038 [9] 196.7 22.1 craters. While impact events lead to the formation of McLaughlin 75 3.7∓0.1 [10] 267.1747.01 steep slopes [3], they are also primarily responsible for Pitiscus 80 3.8∓0.1 [10] 30.57 -50.61 landform degradation [4]. During crater formation, tar- Al-Biruni 80 3.8∓0.1 [10] 92.62 18.09 get properties and processes controlling structural sta- La Pérouse 80 3.6∓0.1 [10] -10.66 76.18 bility limit maximum slopes [4]. -
South Pole-Aitken Basin
Feasibility Assessment of All Science Concepts within South Pole-Aitken Basin INTRODUCTION While most of the NRC 2007 Science Concepts can be investigated across the Moon, this chapter will focus on specifically how they can be addressed in the South Pole-Aitken Basin (SPA). SPA is potentially the largest impact crater in the Solar System (Stuart-Alexander, 1978), and covers most of the central southern farside (see Fig. 8.1). SPA is both topographically and compositionally distinct from the rest of the Moon, as well as potentially being the oldest identifiable structure on the surface (e.g., Jolliff et al., 2003). Determining the age of SPA was explicitly cited by the National Research Council (2007) as their second priority out of 35 goals. A major finding of our study is that nearly all science goals can be addressed within SPA. As the lunar south pole has many engineering advantages over other locations (e.g., areas with enhanced illumination and little temperature variation, hydrogen deposits), it has been proposed as a site for a future human lunar outpost. If this were to be the case, SPA would be the closest major geologic feature, and thus the primary target for long-distance traverses from the outpost. Clark et al. (2008) described four long traverses from the center of SPA going to Olivine Hill (Pieters et al., 2001), Oppenheimer Basin, Mare Ingenii, and Schrödinger Basin, with a stop at the South Pole. This chapter will identify other potential sites for future exploration across SPA, highlighting sites with both great scientific potential and proximity to the lunar South Pole. -
Unravelling the Volcanic History of South Pole-Aitken Basin
42nd Lunar and Planetary Science Conference (2011) 2649.pdf UNRAVELLING THE VOLCANIC HISTORY OF SOUTH POLE-AITKEN BASIN. I. Antonenko1 and G.R. Osinski1, 1Centre for Planetary Science and Exploration & Canadian Lunar Research Network, University of West- ern Ontario, 1151 Richmond St., London, ON, Canada, [email protected]. Introduction: The South Pole-Aitken (SPA) basin is the largest known impact basin on the Moon, located on the south-central farside and measuring approx- imately 2,500 km in diameter [1]. It has been identified as a high priority science target [2], and is the selected destination for the proposed MoonRise sample return mission [3]. Therefore, it is important to understand the geology of SPA, including its volcanic history. Thus motivated, we have begun a large scale study of volcanism in SPA. Our goal is to identify and cha- racterize ancient cryptomare (hidden mare) deposits. We present our results to date. Data: We compiled a variety of different data sets for the central SPA region (Figure 1), including Cle- mentine UVVIS, FeO [4], optical maturity [5], and LOLA topography data, all at a resolution of 1 km/pix. In addition, geologic maps [6,7,8] were corregisted a) and layered on the data. High resolution LROC images were also obtained and examined for selected targets. Method: Cryptomare are generally identified and characterized using dark-haloed craters (DHC’s) [9, 10]. Historically, DHC’s have been identified by the presence of a mature, low albedo halo surrounding an impact crater [9]. However, with the proliferation of new data sets, excavation of basalts can also be identi- fied using the presence of Fe anomalies and basalt spectra in and around craters [10]. -
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America There are approximately 101,135sexual abuse claims filed. Of those claims, the Tort Claimants’ Committee estimates that there are approximately 83,807 unique claims if the amended and superseded and multiple claims filed on account of the same survivor are removed. The summary of sexual abuse claims below uses the set of 83,807 of claim for purposes of claims summary below.1 The Tort Claimants’ Committee has broken down the sexual abuse claims in various categories for the purpose of disclosing where and when the sexual abuse claims arose and the identity of certain of the parties that are implicated in the alleged sexual abuse. Attached hereto as Exhibit 1 is a chart that shows the sexual abuse claims broken down by the year in which they first arose. Please note that there approximately 10,500 claims did not provide a date for when the sexual abuse occurred. As a result, those claims have not been assigned a year in which the abuse first arose. Attached hereto as Exhibit 2 is a chart that shows the claims broken down by the state or jurisdiction in which they arose. Please note there are approximately 7,186 claims that did not provide a location of abuse. Those claims are reflected by YY or ZZ in the codes used to identify the applicable state or jurisdiction. Those claims have not been assigned a state or other jurisdiction. Attached hereto as Exhibit 3 is a chart that shows the claims broken down by the Local Council implicated in the sexual abuse. -
Magnetic Signature of the Lunar South Pole-Aitken Basin: Character, Origin, and Age Michael E
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. ???, XXXX, DOI:10.1029/, Magnetic signature of the lunar South Pole-Aitken Basin: Character, origin, and age Michael E. Purucker,1 and James W. Head III,2 and Lionel Wilson3 Abstract. A new magnetic map of the Moon, based on Lunar Prospector (LP) mag- netometer observations, sheds light on the origin of the South Pole-Aitken Basin (SPA), the largest and oldest of the recognized lunar basins. A set of WNW-trending linear to arcuate magnetic features, evident in both the radial and scalar observations, covers much of a 1000 km wide region centered on the NW portion of SPA. The source bodies are not at the surface because the magnetic features show no first-order correspondence to any surface topographic or structural feature. Patchy mare basalts of possible late Imbrian- age are emplaced within SPA and are inferred to have been emplaced through dikes, di- rectly from mantle sources. We infer that the magnetic features represent dike swarms that served as feeders for these mare basalts, as evident from the location of the Thom- son/Mare Ingenii, Van de Graaff, and Leeuwenhoek mare basalts on the two largest mag- netic features in the region. Modeling suggests that the dike zone is between 25 and 50 km wide at the surface, and dike magnetization contrasts are in the range of 0.2 A/m. We theorize that the basaltic dikes were emplaced in the lunar crust when a long-lived dynamo was active. Based on pressure, temperature, and stress conditions prevalent in the lunar crust, dikes are expected to be a dominantly subsurface phenomenon, consis- tent with the observations reported here.