Asteroid Retrieval Feasibility
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New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period
Hayabusa2 Extended Mission: New Voyage to Rendezvous with a Small Asteroid Rotating with a Short Period M. Hirabayashi1, Y. Mimasu2, N. Sakatani3, S. Watanabe4, Y. Tsuda2, T. Saiki2, S. Kikuchi2, T. Kouyama5, M. Yoshikawa2, S. Tanaka2, S. Nakazawa2, Y. Takei2, F. Terui2, H. Takeuchi2, A. Fujii2, T. Iwata2, K. Tsumura6, S. Matsuura7, Y. Shimaki2, S. Urakawa8, Y. Ishibashi9, S. Hasegawa2, M. Ishiguro10, D. Kuroda11, S. Okumura8, S. Sugita12, T. Okada2, S. Kameda3, S. Kamata13, A. Higuchi14, H. Senshu15, H. Noda16, K. Matsumoto16, R. Suetsugu17, T. Hirai15, K. Kitazato18, D. Farnocchia19, S.P. Naidu19, D.J. Tholen20, C.W. Hergenrother21, R.J. Whiteley22, N. A. Moskovitz23, P.A. Abell24, and the Hayabusa2 extended mission study group. 1Auburn University, Auburn, AL, USA ([email protected]) 2Japan Aerospace Exploration Agency, Kanagawa, Japan 3Rikkyo University, Tokyo, Japan 4Nagoya University, Aichi, Japan 5National Institute of Advanced Industrial Science and Technology, Tokyo, Japan 6Tokyo City University, Tokyo, Japan 7Kwansei Gakuin University, Hyogo, Japan 8Japan Spaceguard Association, Okayama, Japan 9Hosei University, Tokyo, Japan 10Seoul National University, Seoul, South Korea 11Kyoto University, Kyoto, Japan 12University of Tokyo, Tokyo, Japan 13Hokkaido University, Hokkaido, Japan 14University of Occupational and Environmental Health, Fukuoka, Japan 15Chiba Institute of Technology, Chiba, Japan 16National Astronomical Observatory of Japan, Iwate, Japan 17National Institute of Technology, Oshima College, Yamaguchi, Japan 18University of Aizu, Fukushima, Japan 19Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA 20University of Hawai’i, Manoa, HI, USA 21University of Arizona, Tucson, AZ, USA 22Asgard Research, Denver, CO, USA 23Lowell Observatory, Flagstaff, AZ, USA 24NASA Johnson Space Center, Houston, TX, USA 1 Highlights 1. -
Potential Resources on and from the Asteroids/Comets; Threats
ASTEROIDS AND COMETS: POTENTIAL RESOURCES LECTURE 21 NEEP 533 HARRISON H. SCHMITT EROS C-TYPE NASA/NEAR SHOEMAKER/APL 11X11X34 KM ASTEROIDS IN GENERAL 1.3 GM/CM3 MAIN BELT ASTEROIDS BETWEEN JUPITER AND MARS NEAR EARTH ASTEROIDS SOME MAY BE SPENT COMETS EARTH CROSSING ASTEROIDS SOME MAY BE SPENT COMETS “CENTAUR” ASTEROIDS BETWEEN JUPITER AND URANUS CHIRON, 1979 VA, AND 133P/ELST-PIZARRO ALSO HAVE COMET- LIKE BEHAVIOR “TROJAN” ASTEROIDS JUPITER’S ORBIT AND CONTROLLED BY IT GENERAL CHARACTERISTICS RUBBLE PILES (?) NO ASTEROID >150M ROTATES FASTER THAN ONE REVOLUTION PER 2 HOURS CALCULATED LIMIT FOR RUBBLE TO STAY TOGETHER 1998 KY26 IS 30M IN DIAMETER, ROTATES IN 10.7 MIN. AND MAY BE SOLID MAY BE A TRANSITION IN ORBITAL CHARACTERISTICS AND / OR COMPOSITION BETWEEN SOME ASTEROIDS AND COMETS • S-TYPE OTHER ASTEROIDS – INNER ASTEROID BELT – EVIDENCE OF HEATING AND DIFFERENTIATION – 29 TELESCOPIC SPECTRA (Binzel, et al., 1996) • INTERMEDIATE BETWEEN S-TYPE AND ORDINARY CHONDRITES – 1. DISTINCT ROCK TYPES VS DIVERSE LARGER BODIES – 2. ABUNDANCE OF OPAQUE MATERIALS – 3. FRESH SURFACES (MOST LIKELY) • BASALTIC ACHONDRITES (6%) – 4 VESTA AT 2.36 AU [MAIN BELT PARENT (?)] – TOUTATIS - NEA (RADAR STUDY) • 4.5X2.4X1.9KM, 2.1 GM/CM3, TWO ROTATIONS, I.E., TUMBLING (5.4 AND 7.3 DAYS) – 1459 MAGNYA AT 3.15 AU [FRAGMENT OF LARGER BODY (?)] EROS • (Lazzaro, et al, 2000, Science, 288) C-TYPE (REVISED BY GRS DATA) 11X11X33 KM 2.7 GM/CM3 5.27 HR ROTATION NASA/NEAR SHOEMAKER/APL OTHER ASTEROIDS • D-TYPE CARBONACEOUS CHONDRITE (BEYOND MAIN BELT ASTEROIDS) – TAGISH -
Asteroid Retrieval Feasibility Study
Asteroid Retrieval Feasibility Study 2 April 2012 Prepared for the: Keck Institute for Space Studies California Institute of Technology Jet Propulsion Laboratory Pasadena, California 1 2 Authors and Study Participants NAME Organization E-Mail Signature John Brophy Co-Leader / NASA JPL / Caltech [email protected] Fred Culick Co-Leader / Caltech [email protected] Co -Leader / The Planetary Louis Friedman [email protected] Society Carlton Allen NASA JSC [email protected] David Baughman Naval Postgraduate School [email protected] NASA ARC/Carnegie Mellon Julie Bellerose [email protected] University Bruce Betts The Planetary Society [email protected] Mike Brown Caltech [email protected] Michael Busch UCLA [email protected] John Casani NASA JPL [email protected] Marcello Coradini ESA [email protected] John Dankanich NASA GRC [email protected] Paul Dimotakis Caltech [email protected] Harvard -Smithsonian Center for Martin Elvis [email protected] Astrophysics Ian Garrick-Bethel UCSC [email protected] Bob Gershman NASA JPL [email protected] Florida Institute for Human and Tom Jones [email protected] Machine Cognition Damon Landau NASA JPL [email protected] Chris Lewicki Arkyd Astronautics [email protected] John Lewis University of Arizona [email protected] Pedro Llanos USC [email protected] Mark Lupisella NASA GSFC [email protected] Dan Mazanek NASA LaRC [email protected] Prakhar Mehrotra Caltech [email protected] -
The National Aeronautics and Space Administration Planetary Astronomy Program
FRS 347320 FINAL REPORT FOR GRANT NAG5-3938 SUBMITTED TO: The National Aeronautics and Space Administration Planetary Astronomy Program TITLE: Beginning Research with the 1.8-meter Spacewatch Telescope ORGANIZATION: The University of Arizona Lunar and Planetary Laboratory PERIOD OF GRANT: 1996 Dec. 1 - 2000 Nov. 30 PERIOD REPORTED ON: 1996 Dec. I - 2001 Feb. 9 2._o[ PRINCIPAL INVESTIGATOR: Tom Gehrels Date Professor Lunar and Planetary Laboratory University of Arizona Kuiper Space Sciences Building 1629 East University Boulevard Tucson, AZ 85721-0092 Phone: 520/621-6970 FAX: 520/621-1940 Email: [email protected] BUSINESS REPRESENTATIVE: Ms. Lynn A. Lane Senior Business Manager Lunar and Planetary Laboratory University of Arizona Kuiper Space Sciences Building 1629 East University Boulevard Tucson, AZ 85721-0092 Phone: 520/621-6966 FAX: 520/621-4933 Email: [email protected] c:_w_nnsaknag53938.fnl Participating Professionals (all at the Lunar and Planetary Laboratory): Terrence H. Bressi (B. S., Astron. & Physics) Engineer Anne S. Descour (M. S., Computer Science) Senior Systems Programmer Tom Gehrels (Ph. D., Astronomy) Professor, observer, and PI Robert Jedicke (Ph.D., Physics) Principal Research Specialist Jeffrey A. Larsen (Ph. D., Astronomy) Principal Research Specialist and observer Robert S. McMiUan (Ph.D., Astronomy) Associate Research Scientist & observer Joseph L. Montani (M. S., Astronomy) Senior Research Specialist and observer Marcus L. Perry (B. A., Astronomy) (Chief) Staff Engineer James V. Scotti (B. S., Astronomy) Senior Research Specialist and observer PROJECT SUMMARY The purpose of this grant was to bring the Spacewatch 1.8-m telescope to operational status for research on asteroids and comets. -
SPACEWATCH SEARCH for MATERIAL RESOURCES NEAR EARTH Robert S
SPACEWATCH SEARCH FOR MATERIAL RESOURCES NEAR EARTH Robert S. McMillan Lunar & Planetary Laboratory University of Arizona Tucson, AZ Abstract smaller than 100 m. Spacewatch can find the large NEOs while they are as far away as the main asteroid Since 1989 the Spacewatch Project has belt, near the aphelia of their orbits. It is important discovered more than 192 Near-Earth Objects (NEOs). that the discoveries ofNEOs are made with a system of By virtue of a fainter limit of detection compared to known biases and known absolute efficiency so that the other surveys, Spacewatch finds a higher proportion of true distributions versus absolute magnitude and orbital small asteroids (less than 300 meters in diameter). One elements and the total number of objects can be of these, 1998 KY26, is the most accessible to spacecraft extrapolated accurately. The absolute sensitivity and among asteroids with well-known orbits. Spacewatch efficiency of Spacewatch scans have been 10 11 has provided the first- and so far the only- empirical characterized. • information on the critical specific energy and tensile strength of asteroid material. These parameters are With more NEOs found with the well relevant to the mechanics of large-scale mining. Our understood Spacewatch system and more thorough new 1.8-meter telescope will reach a magnitude fainter analyses, more refined understanding of the present than the venerable 0.9-m Spacewatch Telescope. It distributions of NEOs as well as the mechanism by will help NEOs discovered on previous apparitions to which they left the main· belt should be possible. be recovered years later, thus improving knowledge of Spacewatch initially debiased in the four "dimensions" their orbital elements well enough that they will not be of (a, e, i, H), a procedure that is appropriate for · lost. -
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. -
Issue #87 of Lunar and Planetary Information Bulletin
Lunar and Planetary Information BULLETIN Fall 1999/NUMBER 87 • LUNAR AND PLANETARY INSTITUTE • UNIVERSITIES SPACE RESEARCH ASSOCIATION CONTENTS EXTRASOLAR PLANETS THE EFFECT OF PLANET DISCOVERIES ON FACTOR fp NEWS FROM SPACE NEW IN PRINT FIRE IN THE SKY SPECTROSCOPY OF THE MARTIAN SURFACE CALENDAR PREVIOUSPREVIOUS ISSUESISSUES n recent years, headlines have trumpeted the beginning of a I new era in humanity’s exploration of the universe: “A Parade of New Planets” (Scientific American), “Universal truth: Ours EXTRASOLAR Isn’t Only Solar System” (Houston Chronicle), “Three Planets Found Around Sunlike Star” (Astronomy). With more than 20 extrasolar planet or planet candidate discoveries having been announced in the press since 1995 (many PLANETS: discovered by the planet-searching team of Geoff Marcy and Paul Butler of San Francisco State University), it would seem that the detection of planets outside our own solar system has become a commonplace, even routine affair. Such discoveries capture the imagination of the public and the scientific community, in no THE small part because the thought of planets circling distant stars appeals to our basic human existential yearning for meaning. SEARCH In short, the philosophical implication for the discovery of true extrasolar planets (and the ostensible reason why the discovery of FOR extrasolar planets seems to draw such publicity) is akin to when the fictional mariner Robinson Crusoe first spotted a footprint in NEW the sand after 20 years of living alone on a desert island. It’s not exactly a signal from above, but the news of possible extrasolar WORLDS planets, coupled with the recent debate regarding fossilized life forms in martian meteorites, heralds the beginning of a new way of thinking about our place in the universe. -
THE SPACEWATCH PROJECT by Robert S
THE SPACEWATCH PROJECT by Robert S. McMillan Lunar and Planetary Laboratory University of Arizona The Spacewatch Project was begun by Tom After observing for 17 years with an old 0.9- Gehrels and Robert McMillan in 1980 as a scientific meter telescope, Spacewatch has developed a 1.8- exploration of the whole solar system for minor planets meter telescope, the largest in the world dedicated full and comets. Spacewatch pioneered in the use of time to discovering, recovering, and doing astrometry charge-coupled device (CCD) electronic imagery for of asteroids and comets. Astrometric measurements searching and doing astrometry of solar system objects, with this telescope have begun to be reported to the has been scanning the night sky with a ground-based Minor Planet Center. 0.9-meter optical telescope on a regular schedule since Spacewatch has also been developing a 1984, and has been discovering Earth-approaching detector array nine times larger than before to be used Asteroids (EAs) since 1989. on the 0.9-m telescope, which will be upgraded with all Besides being in operation longer than any new optics. This mosaic of CCDs will increase other currently active search program, Spacewatch is Spacewatch's rate of detection of EAs among objects notable for searching fainter than most other EA 2-3 magnitudes fainter than are being found by the surveys. This sensitivity has made it possible for other survey groups. This is an important goal for Spacewatch to discover 23 7 EAs, 16 Centaurs or completing the inventory of even the large EAs. scattered-disk objects, 17 comets, and 7 Trans The advanced technology used by Spacewatch Neptunian Objects (TNOs). -
Hayabusa2 Extended Mission: Rendezvous with 1998 KY26, One of the Most Common but Unexplored Near-Earth Asteroids
EPSC Abstracts Vol. 15, EPSC2021-442, 2021 https://doi.org/10.5194/epsc2021-442 Europlanet Science Congress 2021 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. Hayabusa2 Extended Mission: Rendezvous with 1998 KY26, one of the most common but unexplored near-Earth asteroids Masatoshi Hirabayashi1, Naru Hirata2, Shunichi Kamata3, Kohei Kitazato2, Toru Kouyama4, Tomokatsu Morota5, Naoya Sakatani6, Yuri Shimaki7, Satoshi Tanaka7, Koji Wada8, and Sei-ichiro Watanabe9 1Auburn University, Aerospace Engineering, Auburn, United States of America ([email protected]) 2University of Aizu, Fukushima, Japan 3Hokkaido University, Hokkaido, Japan 4National Institute of Advanced Industrial Science and Technology, Tokyo, Japan 5University of Tokyo, Tokyo, Japan 6Rikkyo University, Tokyo, Japan 7Japan Aerospace Exploration Agency, Kanagawa, Japan 8Chiba Institute of Technology, Chiba, Japan 9Nagoya University, Aichi, Japan Asteroids smaller than a few hundred meters in diameter are generally considered to be the most common in the inner solar system evolution; however, they are usually too faint to be detected. This prevented developing a comprehensive list of them and characterizing their physical and chemical conditions. These small asteroids may be leftovers that survived from their parent bodies' impact- driven catastrophic disruptions (and re-accumulation) or escaped from other planetary bodies during multiple processes. A better understanding of how such objects formed and evolved will constrain the material transport mechanisms in the solar system. Also, smaller asteroids frequently approach the Earth because of their highest population. Some may enter the atmosphere to cause fireball events (they explode while passing through a denser atmosphere) and impact events, leading to damage to civilization. -
Radar and Optical Observations of Asteroid 1998 KY26 Ostro Et Al
Radar and Optical Observations of Asteroid 1998 KY26 Ostro et al. 1 , Radar and Optical Observations of Asteroid 1998 KY26 Steven J. Ostro,'* Petr Pravec,2 Lance A. M. Benner,' R. Scott H~dson,~ Lenka Sarounova,2 Michael D. Hicks,' David L. Rabinowitz,' James V. S~otti,~ David J. Th~len,~Marek Wolf,' Raymond F. Jurgens,' Michael L. Thomas,' Jon D. Giorgini,' Paul W. Chodas,' Donald K. Yeomans,' Randy Rose,' Robert Frye,' Keith D. Rosema,' Ron Winkler,' Martin A. Slade' 'Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91 109-8099, USA. Astronomical Institute, Academy of Sciences of the Czech Republic, CZ-25165 Ondiejov, Czech Republic. 3School of Electrical Engineering and Computer Science, Washington State University, Pullman, Washington99164-2752, USA. Lunar andPlanetary Laboratory, University of Arizona,Tucson, Arizona 85721, USA. Institute forAstronomy, University of Hawaii, 2680 WoodlawnDrive, Honolulu, Hawaii 96822, USA. AstronomicalInstitute, Charles University Prague, V Hol6soviCkach 2, CZ-18000 Prague, Czech Republic. *To whom correspondence should be addressed. E-mail: ostroQreason.jpl.nasa.gov Radar and Optical Observations of Asteroid 1998 KY26 Ostro et al. 2 . Observations of near-Earth asteroid 1998 KY26 shortly after its discovery reveal a slightly elongated spheroidwith a diameter of about 30 m, a compositionanalogous to carbonaceouschondritic meteorites, and a rotation period of 10.7 minutes, which is an order of magnitudeshorter than that measured for anyother solar system object. The rotation is too rapid for 1998 KY26 to consist of multiple componentsbound together just by their mutual gravitational attraction. This monolithic object probably is a fragment derived from cratering or collisional destruction of a much larger asteroid. -
Asteroid Return Mission (Arm)
ASTEROID RETURN MISSION (ARM) 2012 workshop report and ongoing study summary Caltech Keck Institute for Space Studies (KISS) National Research Council presentation 28 March 2013, Washington, DC John Brophy (co-lead), NASA/Caltech-JPL Tom Jones, Florida Institute of Human and Michael Busch, UCLA Machine Cognition Paul Dimotakis (co-lead), Caltech Shri Kulkarni, Caltech Martin Elvis, Harvard-Smithsonian Center for Dan Mazanek, NASA/LaRC Astrophysics Tom Prince, Caltech and JPL Louis Friedman (co-lead), The Planetary Nathan Strange, NASA/Caltech-JPL Society (Emeritus) Marco Tantardini, The Planetary Society Robert Gershman, NASA/Caltech-JPL Adam Waszczak, Caltech Michael Hicks, NASA/Caltech-JPL Don Yeomans, NASA/Caltech-JPL Asteroid-return mission (ARM) study ― I Phase 1: KISS Workshop on the feasibility of an asteroid-capture & return mission • Completed in early 2012 • Study co-leads from Caltech, JPL, and The Planetary Society • Broad invitation and participation (17 national/international organizations) • April 2012 report on the Web Objectives: • Assess feasibility of robotic capture and return of a small near-Earth asteroid to a near-Earth orbit, using technology that can mature in this decade. • Identify potential impacts on NASA and international space community plans for human exploration beyond low-Earth orbit. • Identify benefits to NASA/aerospace and scientific communities, and to the general public. http://www.kiss.caltech.edu/study/asteroid/index.html Asteroid-return mission (ARM) study ― II Phase 2: Three-part follow-on and -
Fast and Slow Rotation of Asteroids
Icarus 148, 12–20 (2000) doi:10.1006/icar.2000.6482, available online at http://www.idealibrary.com on Fast and Slow Rotation of Asteroids Petr Pravec Astronomical Institute, Academy of Sciences of the Czech Republic, CZ-25165 Ondrejov,ˇ Czech Republic E-mail: [email protected] and Alan W. Harris Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, California 91109 Received September 27, 1999; revised December 22, 1999 of rotation rates, both fast and slow, which are most anomalous We present an analysis of the distribution of asteroid spin rates vs. among the smallest asteroids. size. The existence of significant populations of both slow and fast rotators among asteroids smaller than D = 40 km, and especially 2. SPIN DATA below 10 km (where our sample is mostly near-Earth asteroids), is shown. We have found that the excess of slow rotators is present We utilized lists of asteroid periods and lightcurve amplitudes at spin rates below 0.8 rev/day, and the group of fast rotators oc- compiled by A. Harris (version 1997 October) and P. Pravec cupies the range of spin rates >7 rev/day. The fast rotators show (NEAs; version 1999 June). The lists are available from the au- interesting characteristics: The lack of objects rotating faster than thors upon request. From the lists, data for near-Earth asteroids, 2.2 h period among asteroids with absolute magnitude H < 22, as Mars-crossers, and main belt asteroids with quality codes Q 2 well as the tendency to spheroidal shapes of fast rotators, is evi- have been selected; see Harris and Young (1983) for a descrip- dence that asteroids larger than a few hundred meters are mostly tion of the quality codes.