A Chinese / European Exploration Mission to a Binary Near-Earth
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Mars Express Orbiter Radio Science
MaRS: Mars Express Orbiter Radio Science M. Pätzold1, F.M. Neubauer1, L. Carone1, A. Hagermann1, C. Stanzel1, B. Häusler2, S. Remus2, J. Selle2, D. Hagl2, D.P. Hinson3, R.A. Simpson3, G.L. Tyler3, S.W. Asmar4, W.I. Axford5, T. Hagfors5, J.-P. Barriot6, J.-C. Cerisier7, T. Imamura8, K.-I. Oyama8, P. Janle9, G. Kirchengast10 & V. Dehant11 1Institut für Geophysik und Meteorologie, Universität zu Köln, D-50923 Köln, Germany Email: [email protected] 2Institut für Raumfahrttechnik, Universität der Bundeswehr München, D-85577 Neubiberg, Germany 3Space, Telecommunication and Radio Science Laboratory, Dept. of Electrical Engineering, Stanford University, Stanford, CA 95305, USA 4Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91009, USA 5Max-Planck-Instuitut für Aeronomie, D-37189 Katlenburg-Lindau, Germany 6Observatoire Midi Pyrenees, F-31401 Toulouse, France 7Centre d’etude des Environnements Terrestre et Planetaires (CETP), F-94107 Saint-Maur, France 8Institute of Space & Astronautical Science (ISAS), Sagamihara, Japan 9Institut für Geowissenschaften, Abteilung Geophysik, Universität zu Kiel, D-24118 Kiel, Germany 10Institut für Meteorologie und Geophysik, Karl-Franzens-Universität Graz, A-8010 Graz, Austria 11Observatoire Royal de Belgique, B-1180 Bruxelles, Belgium The Mars Express Orbiter Radio Science (MaRS) experiment will employ radio occultation to (i) sound the neutral martian atmosphere to derive vertical density, pressure and temperature profiles as functions of height to resolutions better than 100 m, (ii) sound -
(101955) Bennu from OSIRIS-Rex Imaging and Thermal Analysis
ARTICLES https://doi.org/10.1038/s41550-019-0731-1 Properties of rubble-pile asteroid (101955) Bennu from OSIRIS-REx imaging and thermal analysis D. N. DellaGiustina 1,26*, J. P. Emery 2,26*, D. R. Golish1, B. Rozitis3, C. A. Bennett1, K. N. Burke 1, R.-L. Ballouz 1, K. J. Becker 1, P. R. Christensen4, C. Y. Drouet d’Aubigny1, V. E. Hamilton 5, D. C. Reuter6, B. Rizk 1, A. A. Simon6, E. Asphaug1, J. L. Bandfield 7, O. S. Barnouin 8, M. A. Barucci 9, E. B. Bierhaus10, R. P. Binzel11, W. F. Bottke5, N. E. Bowles12, H. Campins13, B. C. Clark7, B. E. Clark14, H. C. Connolly Jr. 15, M. G. Daly 16, J. de Leon 17, M. Delbo’18, J. D. P. Deshapriya9, C. M. Elder19, S. Fornasier9, C. W. Hergenrother1, E. S. Howell1, E. R. Jawin20, H. H. Kaplan5, T. R. Kareta 1, L. Le Corre 21, J.-Y. Li21, J. Licandro17, L. F. Lim6, P. Michel 18, J. Molaro21, M. C. Nolan 1, M. Pajola 22, M. Popescu 17, J. L. Rizos Garcia 17, A. Ryan18, S. R. Schwartz 1, N. Shultz1, M. A. Siegler21, P. H. Smith1, E. Tatsumi23, C. A. Thomas24, K. J. Walsh 5, C. W. V. Wolner1, X.-D. Zou21, D. S. Lauretta 1 and The OSIRIS-REx Team25 Establishing the abundance and physical properties of regolith and boulders on asteroids is crucial for understanding the for- mation and degradation mechanisms at work on their surfaces. Using images and thermal data from NASA’s Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer (OSIRIS-REx) spacecraft, we show that asteroid (101955) Bennu’s surface is globally rough, dense with boulders, and low in albedo. -
The Terraforming Timeline. A. J. Berliner1 and C. P. Mckay2
Planetary Science Vision 2050 Workshop 2017 (LPI Contrib. No. 1989) 8031.pdf The Terraforming Timeline. A. J. Berliner1 and C. P. McKay2, 1University of California Berkeley, Berkeley, CA 94704, [email protected], 2Space Sciences Division, NASA Ames Research Center, Mountain View, CA 94075. Introduction: Terraforming, the transformation of particularly the winter South Polar Cap, and any CO2 a planet so as to resemble the earth so that it can sup- that is absorbed into the cold ground in the polar re- port widespread life, has been described as a grand gions. Once the warming starts all this releasable CO2 challenge of both space sciences and synthetic biology will go into the atmosphere. Thus, it is important to [1,2]. We propose the following abstract on a Martian know the total before warming starts. Current esti- Terraforming timeline as a guide to shaping planetary mates of the releasable CO2 on Mars today range from science research over the coming century. a little more than the present thin atmosphere to values Terraforming Mars can be divided into two phases. sufficient to create a pressure on Mars equal to the sea The first phase is warming the planet from the present level pressure on Earth. Nitrogen is a fundamental re- average surface temperature of -60ºC to a value close quirement for life and necessary constituent of a to Earth’s average temperature to +15ºC, and re- breathable atmosphere. The recent discovery by the creating a thick CO2 atmosphere [3,4,5,6] This warm- Curiosity Rover of nitrate in the soil on Mars (~0.03% ing phase is relatively easy and quick, and could take by mass) is therefore encouraging for terraforming [7]. -
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, -
Organic Matter and Water from Asteroid Itokawa Q
www.nature.com/scientificreports OPEN Organic matter and water from asteroid Itokawa Q. H. S. Chan1,2*, A. Stephant2, I. A. Franchi2, X. Zhao2, R. Brunetto3, Y. Kebukawa4, T. Noguchi5, D. Johnson2,6, M. C. Price7, K. H. Harriss7, M. E. Zolensky8 & M. M. Grady2,9 Understanding the true nature of extra-terrestrial water and organic matter that were present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which was the frst mission that brought pristine asteroidal materials to Earth’s astromaterial collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD = + 4868 ± 2288‰; δ15N = + 344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and ofers support for material mixing in the asteroid belt that occurred in scales from small dust infall to catastrophic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modifed by D-enriched exogenous organics and water derived from a carbonaceous parent body. Understanding the earliest chemical reactions involving liquid water provides crucial insights to how simple building blocks of organic compounds evolved into increasingly complex macromolecules via actions of water. -
Abstracts of the 50Th DDA Meeting (Boulder, CO)
Abstracts of the 50th DDA Meeting (Boulder, CO) American Astronomical Society June, 2019 100 — Dynamics on Asteroids break-up event around a Lagrange point. 100.01 — Simulations of a Synthetic Eurybates 100.02 — High-Fidelity Testing of Binary Asteroid Collisional Family Formation with Applications to 1999 KW4 Timothy Holt1; David Nesvorny2; Jonathan Horner1; Alex B. Davis1; Daniel Scheeres1 Rachel King1; Brad Carter1; Leigh Brookshaw1 1 Aerospace Engineering Sciences, University of Colorado Boulder 1 Centre for Astrophysics, University of Southern Queensland (Boulder, Colorado, United States) (Longmont, Colorado, United States) 2 Southwest Research Institute (Boulder, Connecticut, United The commonly accepted formation process for asym- States) metric binary asteroids is the spin up and eventual fission of rubble pile asteroids as proposed by Walsh, Of the six recognized collisional families in the Jo- Richardson and Michel (Walsh et al., Nature 2008) vian Trojan swarms, the Eurybates family is the and Scheeres (Scheeres, Icarus 2007). In this theory largest, with over 200 recognized members. Located a rubble pile asteroid is spun up by YORP until it around the Jovian L4 Lagrange point, librations of reaches a critical spin rate and experiences a mass the members make this family an interesting study shedding event forming a close, low-eccentricity in orbital dynamics. The Jovian Trojans are thought satellite. Further work by Jacobson and Scheeres to have been captured during an early period of in- used a planar, two-ellipsoid model to analyze the stability in the Solar system. The parent body of the evolutionary pathways of such a formation event family, 3548 Eurybates is one of the targets for the from the moment the bodies initially fission (Jacob- LUCY spacecraft, and our work will provide a dy- son and Scheeres, Icarus 2011). -
A New Era for AI, Human-Robotic Interactions (HRI), and Multidisciplinary Social Science?
International Robotics & Automation Journal Research Article Open Access Terra forming of social systems and human behavior: a new era for AI, human-robotic interactions (HRI), and multidisciplinary social science? Abstract Volume 6 Issue 4 - 2020 This mini-script seeks to generate concerns around an emerging field of work related Édgar Giovanni Rodríguez Cuberos to space exploration and the rest of society generated by the idea of human colonies in Facultad de Ciencias de la Educación, Fundación Universitaria extraterrestrial environments (space stations, moons, and planets). There exists abundant Juan de Castellanos, Colombia literature on terraforming from biogeochemical conditions, however, there is very limited research about human behavior, interactions, and specific studies of relationships with Correspondence: Édgar Giovanni Rodríguez Cuberos, robots and artificial intelligence into the environments presented previously. For this Facultad de Ciencias de la Educación, Humanidades y Artes, reason, and with the intention of not replicating the same problems derived from our human Fundación Universitaria Juan de Castellanos, Tunja –Colombia, condition (violence, extractivism, corruption, etc) preliminary ideas are exposed to think Email and contribute to the emerging field of cosmoeducation or exo-humanities and others “exo –disciplines” oriented to alternated social systems and human behavioral for a new era of Received: August 20, 2020 | Published: December 17, 2020 exploration. Keywords: AI ethics, human robot interactions (HRI), social terraforming, exohumanities, posthumanities Introduction of supporting Earth-like life, however, the looming ecological consequences of human activities suggest that in the decades to come “When you eliminate the impossible, what remains, while we might need to terraform our own planet if it is to remain a viable improbable, must be the truth.” host for Earth-like life.” Mr. -
Evolution of Dust Particles Ejected by Catastrophic Asteroidal Disruptions
EVOLUTION OF DUST PARTICLES EJECTED BY CATASTROPHIC ASTEROIDAL DISRUPTIONS Thomas Kehoe, Stanley Dermott, Ashley Espy Department of Astronomy, University of Florida The contribution of asteroidal dust to the zodiacal cloud has previously been discussed in terms of a collisional cascade process, whereby dust is produced by the grinding down of large objects. However, there is now evidence that debris disks, such as the zodiacal cloud, are refreshed stochastically by the injection of dust produced by the catastrophic collisional breakup of a large planetesimal. Asteroid families provide dramatic proof of the occurrence of such collisions in the solar system. There are now known to be at least two examples of asteroids, tens to hundreds of kilometers in diameter, that have been catastrophically disrupted by an impact within the last ten million years. These collisional events resulted in the creation of the Veritas family and the Karin cluster. Enormous quantities of dust are injected into the zodiacal cloud following such family-forming impact events and the remnants of the collisional debris produced by these disruptions can still be observed today in the form of dust bands. Following its production, this material evolves both dynamically and collisionally, with the result that a wave of dust particles is transported from its source region in the asteroid belt into the inner solar system Evidence shows that many asteroids are not coherent, solid bodies but are instead highly fractured, highly porous, and only loosely bound by gravity. Dust may be generated by im- pact processes in the regoliths of such ”rubble piles” and so the contribution of asteroidal dust to the zodiacal cloud may be determined by a quite different mechanism to the col- lisional cascade process, with only a few rubble piles providing the majority of asteroidal dust in the solar system at any particular epoch. -
Educator's Guide
educator’s guide Table of Contents INTRODUCTION . 3 ACTIVITY FOR GRADES 3-5 Introduction for Educator . 4 Asteroids in Orbit Student Activity . 5 ACTIVITIES FOR GRADES 6-8 Introduction for Educator . 7 What Are Asteroids? Instructions for Educator . 7 Making a Splash Instructions for Educator . 7 Working Together Instructions for Educator . 8 What Are Asteroids? Student Activity . 9 Making a Splash Student Activity . 11 Working Together Student Activity . 13 ACTIVITIES FOR GRADES 9-12 Introduction for Educator . 15 Tracing the Past Instructions for Educator . 15 Defending the Future Instructions for Educator . 16 Tracing the Past Student Activity . 17 Defending the Future Student Activity . 18 EDUCATIONAL STANDARDS ALIGNMENT . 19 ACKNOWLEDGEMENTS . 20 2 Introduction AN EXTRAORDINARY FIELD TRIP AND LEARNING EXPERIENCE! Dear Educator, Planetary defense is a relatively new science . Only a few decades ago did we become certain Earth’s history of asteroid impacts was sure to repeat itself . Could we save our world today from a cosmic threat? You bet we can . But to tend to this problem, we must first understand it . That’s where Asteroid Hunters comes in . Asteroid Hunters will take your students on an exciting field trip across the Solar System and to the dawn of time . They’ll watch how gravity spun gas and dust into our Solar System, how rocky debris gathered into worlds, and how the planet-building leftovers became asteroids . They’ll learn that these natural wonders of deep space brought water to planets, and the building blocks of life itself . They will also see how we possess the technological know-how to keep an asteroid from hitting our planet– unlike the doomed dinosaurs of 65 million years ago . -
X-Rays Studies of the Solar System (Thematic Area: Planetary Systems)
X-rays Studies of the Solar System (Thematic Area: Planetary Systems) Bradford Snios1,∗, William R. Dunn1,2,∗, Carey M. Lisse3, Graziella Branduardi-Raymont2, Konrad Dennerl4, Anil Bhardwaj5, G. Randall Gladstone6, Susan Nulsen1, Dennis Bodewits7, Caitriona M. Jackman8, Julián D. Alvarado-Gómez1, Emma J. Bunce9, Michael R. Combi10, Thomas E. Cravens11, Renata S. Cumbee12, Jeremy J. Drake1, Ronald F. Elsner13, Denis Grodent14, Jae Sub Hong1, Vasili Kharchenko1,15, Ralph P. Kraft1, Joan P. Marler16, Sofia P. Moschou1, Patrick D. Mullen17, Scott J. Wolk1, Zhonghua Yao14 1. Center for Astrophysics | Harvard & Smithsonian, Cambridge, MA, USA 2. University College London, London, UK 3. Johns Hopkins University Applied Physics Laboratory, Laurel, MD, USA 4. Max-Planck-Institut für extraterrestrische Physik, Garching, Germany 5. Physical Research Laboratory, Ahmedabad, India 6. Southwest Research Institute, San Antonio, TX, USA 7. Auburn University, Auburn, AL 8. University of Southampton, Southampton, UK 9. University of Leicester, Leicester, UK 10. University of Michigan, Ann Arbor, MI, USA 11. University of Kansas, Lawrence, KS, USA 12. NASA Goddard Space Flight Center, Greenbelt, MD, USA 13. NASA Marshall Space Flight Center, Huntsville, AL, USA 14. Université de Liège, Liège, Belgium 15. University of Connecticut, Storrs, CT, USA 16. Clemson University, Clemson, SC, USA 17. University of Illinois Urbana-Champaign, Champaign, IL, USA X-ray observatories contribute fundamental advances in Solar System studies by prob- ing Sun-object interactions, developing planet and satellite surface composition maps, probing global magnetospheric dynamics, and tracking astrochemical reactions. Despite these crucial results, the technological limitations of current X-ray instruments hinder the overall scope and impact for broader scientific application of X-ray observations both now and in the coming decade. -
Is Asteroid 2002Ny40 a Rubble Pile Gravitationally Disrupted? J
Lunar and Planetary Science XXXIX (2008) 1692.pdf IS ASTEROID 2002NY40 A RUBBLE PILE GRAVITATIONALLY DISRUPTED? J. M. Trigo-Rodríguez1,2, W.F. Bottke3, A. Campo Bagatin4, P. Tanga5, J. Llorca6, D.C. Jones7, I.P. Williams7, J.M. Madiedo8, and E. Lyytinen9. 1Institute of Space Sciences (CSIC). Campus UAB, Facultat de Ciències, Torre C5-2ª planta. 08193 Bellaterra, Spain; 2Institut d’Estudis Espacials de Catalunya. Gran Capità 2-4, Ed. Nexus. 08034 Bar- celona, Spain; 3 Southwest Research Institute, Boulder, Colorado, USA; 4 Universidad de Alicante, Spain; 5 Obser- vatoire de Nice, France; 6 Institut de Tècniques Energètiques, Universitat Politècnica de Catalunya (UPC), Barce- lona; 7 Astronomy Unit, Queen Mary University of London, London, United Kingdom; 8 Facultad de Ciencias, Uni- versidad de Huelva, Spain; 9 Finish Fireball Network, Kehäkukantie 3B, 00720 Helsinki, Finland. Introduction: The existence of meteoroid streams Results and discussion: Due to the relative low containing meter-sized meteoroids capable of produc- population of the NEO region, a collision among as- ing meteorites after atmospheric interaction was pro- teroids is an unlikely, but not negligible process for posed quite recently [1]. Their existence has important producing the observed asteroidal fragments. In any implications because they can be naturally delivering case, we have searched for alternative processes capa- to the Earth different types of rock-forming materials ble of producing the meteoroid stream. a) One option from Potentially Hazardous Asteroids (PHA). would be that the meteoroids were ejected by a fast rotator, unlikely according to the present spin of both The recent identification of Near Earth Object asteroids, but not taking into account the YORP effect. -
Small Solar System Bodies As Granular Media D
Small Solar System Bodies as granular media D. Hestroffer, P. Sanchez, L Staron, A. Campo Bagatin, S. Eggl, W. Losert, N. Murdoch, E. Opsomer, F. Radjai, D. C. Richardson, et al. To cite this version: D. Hestroffer, P. Sanchez, L Staron, A. Campo Bagatin, S. Eggl, et al.. Small Solar System Bodiesas granular media. Astronomy and Astrophysics Review, Springer Verlag, 2019, 27 (1), 10.1007/s00159- 019-0117-5. hal-02342853 HAL Id: hal-02342853 https://hal.archives-ouvertes.fr/hal-02342853 Submitted on 4 Nov 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Astron Astrophys Rev manuscript No. (will be inserted by the editor) Small solar system bodies as granular media D. Hestroffer · P. S´anchez · L. Staron · A. Campo Bagatin · S. Eggl · W. Losert · N. Murdoch · E. Opsomer · F. Radjai · D. C. Richardson · M. Salazar · D. J. Scheeres · S. Schwartz · N. Taberlet · H. Yano Received: date / Accepted: date Made possible by the International Space Science Institute (ISSI, Bern) support to the inter- national team \Asteroids & Self Gravitating Bodies as Granular Systems" D. Hestroffer IMCCE, Paris Observatory, universit´ePSL, CNRS, Sorbonne Universit´e,Univ.