Near Earth Asteroid Thermal Modeling
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Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa
dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966 Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D. -
Near Earth Asteroid Rendezvous: Mission Summary 351
Cheng: Near Earth Asteroid Rendezvous: Mission Summary 351 Near Earth Asteroid Rendezvous: Mission Summary Andrew F. Cheng The Johns Hopkins Applied Physics Laboratory On February 14, 2000, the Near Earth Asteroid Rendezvous spacecraft (NEAR Shoemaker) began the first orbital study of an asteroid, the near-Earth object 433 Eros. Almost a year later, on February 12, 2001, NEAR Shoemaker completed its mission by landing on the asteroid and acquiring data from its surface. NEAR Shoemaker’s intensive study has found an average density of 2.67 ± 0.03, almost uniform within the asteroid. Based upon solar fluorescence X-ray spectra obtained from orbit, the abundance of major rock-forming elements at Eros may be consistent with that of ordinary chondrite meteorites except for a depletion in S. Such a composition would be consistent with spatially resolved, visible and near-infrared (NIR) spectra of the surface. Gamma-ray spectra from the surface show Fe to be depleted from chondritic values, but not K. Eros is not a highly differentiated body, but some degree of partial melting or differentiation cannot be ruled out. No evidence has been found for compositional heterogeneity or an intrinsic magnetic field. The surface is covered by a regolith estimated at tens of meters thick, formed by successive impacts. Some areas have lesser surface age and were apparently more recently dis- turbed or covered by regolith. A small center of mass offset from the center of figure suggests regionally nonuniform regolith thickness or internal density variation. Blocks have a nonuniform distribution consistent with emplacement of ejecta from the youngest large crater. -
Asteroids Upclose
Asteroids UpClose Quick Views of Big Advances Asteroids Up Close The importance of spacecraft missions in the quest to understand asteroids is highlighted in a recent review paper by Thomas Burbine (Mount Holyoke College, Massachusettes). Burbine discusses achievements in understanding the chemistries and mineralogies of asteroids since the launch of NASA's NEAR-Shoemaker robotic spacecraft in 1996, the first mission dedicated to asteroid exploration. As two new robotic asteroid-sample-return missions are underway (NASA's OSIRIS-REx and JAXA's Hayabusa2), Burbine's review paper and a review by Derek Sears earlier this year (see the January 2016 PSRD CosmoSparks: Comprehending Asteroids) provide timely recaps of why asteroids are so important to our understanding of the building Simulated cratering and topography are overlaid on blocks of our Solar System. radar imagery of asteroid Bennu — one of the next asteroids to be visited up close by NASA's OSIRIS- Burbine reviews these mission highlights: REx mission. Click image for more information from University of Arizona News. NEAR-Shoemaker (NASA mission) flew by (253) Mathilde, a C-complex asteroid. It orbited and landed on (433) Eros, an S-type asteroid, and used an X-ray spectrometer to determine elemental ratios, which were consistent with a body that did not melt globally. Most likely meteorite matches for Eros are surface-altered ordinary chondrites or primitive achondrites. For more see PSRD article: The Composition of Asteroid 433 Eros. Hayabusa (JAXA mission) was a touch-and-go mission to (25143) Itokawa, an S-complex asteroid. It carried a multiband imager, near-infrared spectrometer, laser altimeter, LIDAR, X-ray spectrometer, and a sample capsule. -
Final Report Asteroid Impact Monitoring
Final Report Asteroid Impact Monitoring Environmental and Instrumentation Requirements A component of the Asteroid Impact & Deflection Assessment (AIDA) Mission By the AIM Advisory Team Dr. Patrick MICHEL (Univ. Nice, CNRS, OCA), Team Leader Dr. Jens Biele (DLR) Dr. Marco Delbo (Univ. Nice, CNRS, OCA) Dr. Martin Jutzi (Univ. Bern) Pr. Guy Libourel (Univ. Nice, CNRS, OCA) Dr. Naomi Murdoch Dr. Stephen R. Schwartz (Univ. Nice, CNRS, OCA) Dr. Stephan Ulamec (DLR) Dr. Jean-Baptiste Vincent (MPS) April 12th, 2014 Introduction In this report, we describe the knowledge gain resulting from the implementation of either the European Space Agency’s Asteroid Impact Monitoring (AIM) as a stand- alone mission or AIM with its second component, the Double Asteroid Redirection Test (DART) mission under study by the Johns Hopkins Applied Physics Laboratory with support from members of NASA centers including Goddard Space Flight Center, Johnson Space Center, and the Jet Propulsion Laboratory. We then present our analysis of the required measurements addressing the goals of the AIM mission to the binary Near-Earth Asteroid (NEA) Didymos, and for two specified payloads. The first payload is a mini thermal infrared camera (called TP1) for short and medium range characterisation. The second payload is an active seismic experiment (called TP2). We then present the environmental parameters for the AIM mission. AIM is a rendezvous mission that focuses on the monitoring aspects i.e., the capability to determine in-situ the key properties of the secondary of a binary asteroid. DART consists primarily of an artificial projectile aims to demonstrate asteroid deflection. In the framework of the full AIDA concept, AIM will also give access to the detailed conditions of the DART impact and its outcome, allowing for the first time to get a complete picture of such an event, a better interpretation of the deflection measurement and a possibility to compare with numerical modeling predictions. -
Daniel J. Scheeres, Phd. Degrees Professional Positions
Daniel J. Scheeres, PhD. University of Colorado Distinguished Professor A. Richard Seebass Endowed Chair Celestial and Spaceflight Mechanics Laboratory Head Colorado Center for Astrodynamics Research Member Address: 429 UCB, Boulder, CO 80309-0429 USA Office: ECOT 611 Tel: (720) 544-1260, Fax: (303) 492-7881 Website: ccar.colorado.edu/scheeres [email protected] Degrees Ph.D. Aerospace Engineering The University of Michigan, 1992 On symmetric central configurations with application to satellite motion about rings Prof. N.X. Vinh, Chairman. M.S.E. Aerospace Engineering The University of Michigan, 1988 B.S.E. Aerospace Engineering (summa cum laude) The University of Michigan, 1987 B.S. Letters and Engineering Calvin College, 1985 Professional Positions The University of Colorado Boulder Ann & H.J. Smead Department of Aerospace Engineering Sciences University of Colorado Distinguished Professor 11/14 { present A. Richard Seebass Endowed Chair Professor 2/08 { present Associate Chair for Graduate Studies 7/13 { 6/15 Visiting Professor 8/07 { 2/08 The University of Michigan Department of Aerospace Engineering Adjunct Professor 2/08 { 9/10 Graduate Chair, Department of Aerospace Engineering 10/06 { 12/07 Associate Professor 9/02 { 1/08 Assistant Professor 9/99 { 8/02 Institute of Space and Astronautical Science, Japan Visiting Professor, JSPS Fellow 8/05 { 12/05 Japan Society for the Promotion of Science Fellow 5/99 { 8/99 Iowa State University Department of Aerospace Engineering and Engineering Mechanics Assistant Professor 8/97 { 8/99 Daniel J. Scheeres, PhD. 1 September 18, 2017 Jet Propulsion Laboratory, California Institute of Technology Senior Member of Engineering Staff 3/97 { 7/97 Member of the Technical Staff 9/92 { 3/97 Summer Intern/On-call employee 5/89 { 9/92 Honors and awards • 2017 Department of Aerospace Engineering Sciences Faculty Award for Outstanding Re- search ($1,000 Award). -
The Landing of the NEAR-Shoemaker Spacecraft on Asteroid 433 Eros
letters to nature ................................................................. images were buffered in real-time and then played back while the next The landing of the NEAR-Shoemaker set was being acquired. All images were shuttered using an exposure of 15 ms to limit smear. Here we summarize the major insights spacecraft on asteroid 433 Eros about the surface of Eros obtained from the images. More detailed analyses of speci®c observations are provided in accompanying 5 4 J. Veverka*, B. Farquhar², M. Robinson³, P. Thomas*, S. Murchie², contributions describing ponded deposits and ejecta blocks . A. Harch*, P. G. Antreasian§, S. R. Chesley§, J. K. Miller§, The selection of the landing site was dictated by several practical W. M. Owen Jr§, B. G. Williams§, D. Yeomans§, D. Dunham², G. Heyler², considerations that are summarized in the legend to Fig. 1. One aim M. Holdridge², R. L. Nelson², K. E. Whittenburg², J. C. Ray², B. Carcich*, was to land the NEAR spacecraft in a region where details of surface A. Cheng², C. Chapmank, J. F. Bell III*, M. Bell*, B. Bussey³, B. Clark*, modi®cation by ejecta and downslope movement of regolith could D. Domingue², M. J. Gaffey¶, E. Hawkins², N. Izenberg², J. Joseph*, be studied. We hoped to land in the vicinity of one of the enigmatic R. Kirk#, P. LuceyI, M. Malin**, L. McFadden²², W. J. Merlinek, `ponds' discovered during the 28 October 2000 low-altitude ¯yby6 C. Peterson*, L. Prockter², J. Warren² & D. Wellnitz²² and viewed at even better resolution (0.5 m) in late January 2001. The location of the landing site, within the 9-km depression * Space Sciences Building, Cornell University, Ithaca, New York 14853, USA Himeros, is shown in Fig. -
An Innovative Solution to NASA's NEO Impact Threat Mitigation Grand
Final Technical Report of a NIAC Phase 2 Study December 9, 2014 NASA Grant and Cooperative Agreement Number: NNX12AQ60G NIAC Phase 2 Study Period: 09/10/2012 – 09/09/2014 An Innovative Solution to NASA’s NEO Impact Threat Mitigation Grand Challenge and Flight Validation Mission Architecture Development PI: Dr. Bong Wie, Vance Coffman Endowed Chair Professor Asteroid Deflection Research Center Department of Aerospace Engineering Iowa State University, Ames, IA 50011 email: [email protected] (515) 294-3124 Co-I: Brent Barbee, Flight Dynamics Engineer Navigation and Mission Design Branch (Code 595) NASA Goddard Space Flight Center Greenbelt, MD 20771 email: [email protected] (301) 286-1837 Graduate Research Assistants: Alan Pitz (M.S. 2012), Brian Kaplinger (Ph.D. 2013), Matt Hawkins (Ph.D. 2013), Tim Winkler (M.S. 2013), Pavithra Premaratne (M.S. 2014), Sam Wagner (Ph.D. 2014), George Vardaxis, Joshua Lyzhoft, and Ben Zimmerman NIAC Program Executive: Dr. John (Jay) Falker NIAC Program Manager: Jason Derleth NIAC Senior Science Advisor: Dr. Ronald Turner NIAC Strategic Partnerships Manager: Katherine Reilly Contents 1 Hypervelocity Asteroid Intercept Vehicle (HAIV) Mission Concept 2 1.1 Introduction ...................................... 2 1.2 Overview of the HAIV Mission Concept ....................... 6 1.3 Enabling Space Technologies for the HAIV Mission . 12 1.3.1 Two-Body HAIV Configuration Design Tradeoffs . 12 1.3.2 Terminal Guidance Sensors/Algorithms . 13 1.3.3 Thermal Protection and Shield Issues . 14 1.3.4 Nuclear Fuzing Mechanisms ......................... 15 2 Planetary Defense Flight Validation (PDFV) Mission Design 17 2.1 The Need for a PDFV Mission ............................ 17 2.2 Preliminary PDFV Mission Design by the MDL of NASA GSFC . -
Dawn Mission Reveals Dwarf Planet Else in the Solar System
Fossil Planet With lowlands, highlands, weird white spots, and even a pyramid, the largest object in the asteroid belt is unlike anything Dawn mission reveals dwarf planet else in the solar system. by Eric Betz IN THE BEGINNING, with a mass equivalent to just 4 percent of that contained in Earth’s Moon. What was OUR SOLAR SYSTEM left is what we still see today. One-third of that mass is held by a single WAS A VIOLENT PLACE. world, Ceres. At 590 miles (950 kilometers) NASA’s Dawn mission Radiation from neighboring massive across, it’s our solar system’s largest asteroid captured Ceres from stars bombarded our small part of a large and the only dwarf planet this side of Pluto. Ceres 8,400 miles (13,600 kilometers) away in molecular cloud — a many light-years-wide It’s also a relic of our violent origins. May as it spiraled body of gas and dust resembling the Eagle This icy body is the current focus of into ever-lower Nebula’s “Pillars of Creation” — as the NASA’s Dawn mission — a small spacecraft orbits. ALL IMAGES: NASA/ JPL-CALTECH/UCLA/MPS/DLR/IDA, whole expanse coalesced like a figure skater that’s powered its way across the inner solar EXCEPT WHERE NOTED pulling her limbs in tight for a spin. system since 2007 using unconventional Some 99.8 percent of the mass drew to ion propulsion. The engine allowed Dawn the center, forming our Sun. And out of the to become the first mission to ever orbit firmament 4.6 billion years ago, tiny bits of two extraterrestrial bodies. -
– Near-Earth Asteroid Mission Concept Study –
ASTEX – Near-Earth Asteroid Mission Concept Study – A. Nathues1, H. Boehnhardt1 , A. W. Harris2, W. Goetz1, C. Jentsch3, Z. Kachri4, S. Schaeff5, N. Schmitz2, F. Weischede6, and A. Wiegand5 1 MPI for Solar System Research, 37191 Katlenburg-Lindau, Germany 2 DLR, Institute for Planetary Research, 12489 Berlin, Germany 3 Astrium GmbH, 88039 Friedrichshafen, Germany 4 LSE Space AG, 82234 Oberpfaffenhofen, Germany 5 Astos Solutions, 78089 Unterkirnach, Germany 6 DLR GSOC, 82234 Weßling, Germany ASTEX Marco Polo Symposium, Paris 18.5.09, A. Nathues - 1 Primary Objectives of the ASTEX Study Identification of the required technologies for an in-situ mission to two near-Earth asteroids. ¾ Selection of realistic mission scenarios ¾ Definition of the strawman payload ¾ Analysis of the requirements and options for the spacecraft bus, the propulsion system, the lander system, and the launcher ASTEX ¾ Definition of the requirements for the mission’s operational ground segment Marco Polo Symposium, Paris 18.5.09, A. Nathues - 2 ASTEX Primary Mission Goals • The mission scenario foresees to visit two NEAs which have different mineralogical compositions: one “primitive'‘ object and one fragment of a differentiated asteroid. • The higher level goal is the provision of information and constraints on the formation and evolution history of our planetary system. • The immediate mission goals are the determination of: – Inner structure of the targets – Physical parameters (size, shape, mass, density, rotation period and spin vector orientation) – Geology, mineralogy, and chemistry ASTEX – Physical surface properties (thermal conductivity, roughness, strength) – Origin and collisional history of asteroids – Link between NEAs and meteorites Marco Polo Symposium, Paris 18.5.09, A. -
Lecture 2: Course Overview Introduction to the Solar System
Lecture 2: Course Overview Introduction to the Solar System AST2003 Section 6218 - Spring 2012 Instructor: Professor Stanley F. Dermott Office: 216 Bryant Space Science Center Phone: 352 294 1864 email [email protected] Lecture time and place: Tuesdays (4th period: 10:40 am – 11:30 am) Thursdays (4th and 5th period) (10:40 am – 12:35 pm), FLG 210 Office hours: Tuesdays 11:45 – 12:45 pm, Thursdays 12:45 pm - 1:45 pm or by appointment Teacher Assistant: Dr Naibi Marinas (Help with Mastering Astronomy and Exam Reviews) Office: 312 Bryant Space Science Center Phone: 325 294 1848 Email: [email protected]!! Class Website: http://www.astro.ufl.edu/~marinas/astro/AST2003.html A bit about myself Russian Translation Worked with Carl Sagan while at Cornell Carl Sagan: Author and presenter of COSMOS Two papers in Nature Radar images of hydrocarbon lakes on Titan taken by Cassini spacecraft This movie, comprised of several detailed images taken by Cassini's radar instrument, shows bodies of liquid near Titan's north pole. Biggest Discovery! Published in Nature in 1994 © 1994 Nature Publishing Group © 1994 Nature Publishing Group © 1994 Nature Publishing Group Last sentence in the paper © 1994 Nature Publishing Group Structure in Debris Disks Structure in Debris DebrisDisks disks imply >km planetesimals around Debris disks imply >km main sequence stars, but planetesimals around also evidence for planets: main sequence stars, but •! inner regions are empty, also evidence for planets: probably cleared by planet formation •! inner regions are empty, -
The Spin State of 433 Eros and Its Possible Implications
Icarus 175 (2005) 419–434 www.elsevier.com/locate/icarus The spin state of 433 Eros and its possible implications D. Vokrouhlický a,∗,W.F.Bottkeb, D. Nesvorný b a Institute of Astronomy, Charles University, V Holešoviˇckách 2, CZ-18000 Prague 8, Czech Republic b Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, CO 80302, USA Received 10 September 2004; revised 16 November 2004 Available online 3 March 2005 Abstract In this paper, we show that Asteroid (433) Eros is currently residing in a spin–orbit resonance, with its spin axis undergoing a small- amplitude libration about the Cassini state 2 of the proper mode in the nonsingular orbital element sin I/2exp(ıΩ),whereI the orbital inclination and Ω the longitude of the node. The period of this libration is 53.4 kyr. By excluding these libration wiggles, we find that Eros’ pole precesses with the proper orbital plane in inertial space with a period of 61.4 kyr. Eros’ resonant state forces its obliquity to oscillate ◦ ◦ ◦ with a period of 53.4 kyr between 76 and 89.5 . The observed value of 89 places it near the latter extreme of this cycle. We have used these results to probe Eros’ past orbit and spin evolution. Our computations suggest that Eros is unlikely to have achieved its current spin state by solar and planetary gravitational perturbations alone. We hypothesize that some dissipative process such as thermal torques (e.g., the so-called YORP effect) may be needed in our model to obtain a more satisfactory match with data. -
NASA Workshop on Scientific Requirements for Mitigation of Hazardous Comets and Asteroids
Extended Abstracts from the NASA Workshop on Scientific Requirements for Mitigation of Hazardous Comets and Asteroids held in Arlington, VA September 3-6, 2002 Erik Asphaug and Nalin Samarasinha, eds. [email protected], [email protected] October 24, 2002 Workshop Poster (July 2002) NOTE: The abstracts contained herein are compiled as received from the authors, with no modification other than file conversion to PDF and concatenation into a single document. No effort has been made to rectify any aspect of any submission, other than to ensure that the proper author heading appears on the associated pages. This document may be freely transmitted in its entirety. Individual authors maintain copyright ownership to their submitted works. In September 2002, NASA’s Office of Space Science sponsored a workshop on Scientific Requirements for Mitigation of Hazardous Comets and Asteroids, attended by 70 scientists from around the world and 20 registered media participants. Peer reviewed invited proceedings from this workshop will be published by Cambridge University Press in late 2003; extended abstracts from both invited and contributed talks are included here. See http://www.noao.edu/meetings/mitigation for updates on the book publication and for other materials related to the workshop. This document will be archived at the above site, and may be updated in time with better formatting. In addition to NASA’s sponsorship, support from Ball Aerospace, NOAO, The University of Maryland, Lockheed Martin and SAIC helped make the workshop a success and is gratefully acknowledged. On the following pages you will find the consensus statement that was released to the press on the final day of the workshop, followed by contributed extended abstracts in alphabetical order.