The Hathor Excavator: a Mission Proposal for Asteroid Mining and the Space Launch System
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REASONS to MIND ASTEROIDS with the Rapid Progress Made In
ASTEROID MINING & ITS LEGAL IMPLICATIONS Neil Modi & Devanshu Ganatra Presentation ID- IAC- 16.E7.IP.23.x32357 REASONS TO MINE ASTEROIDS With the rapid progress made in technology, humans are taking huge steps in space today. There is huge potential in space, and particularly in asteroid mining. ENERGY CRISIS RARE EARTH METALS • Non-renewable fossil fuels like coal, oil currently account for 81% of • Many of the metals widely used in almost all industrial products the world’s primary energy. were always limited and are now in SHORT SUPPLY leading to skyrocketing manufacturing costs. • EARLIER, renewable energy could not compete with non-renewable sources because it relied on metals in short supply. Resources found • These include Platinum Group Metals (PMGS) and others like on asteroids would solve this problem completely. gold, cobalt, iron, molybdenum etc. Image Credit-The U.S. Energy Image Credit- FuelSpace.org- ‘How Asteroids Can Information Administration Save Mankind’ PROJECTED SCARCITY OF RESOURCES ON EARTH Image Credit-Shackleton Energy Company Image Credit- Chris Clugston’s ‘An Oil Drum- An Analysis’ (2010) THE NEED FOR WATER 1. SUPPORT SYSTEM FOR ASTRONAUTS- Since the main constituents of water HYDRATION AND OXYGEN are hydrogen and oxygen, it is a source of oxygen for life support. TO ASTRONAUTS 2. PROTECTION FROM RADIATION- Water absorbs and blocks infrared radiation, which means that by storing heat it helps to maintain temperature. 3. ROCKET FUEL- Rocket propellant is hydrogen and oxygen based, with a large percentage of the weight of a spacecraft taken up by fuel. 4. SPACE EXPLORATION- A GAS STATION IN SPACE KEY TO SPACE BLOCKS EXPLORATION WATER RADIATION Today billions of dollars are spent in rocket fuel to sustain space explorations. -
Asteroid Retrieval Mission
Where you can put your asteroid Nathan Strange, Damon Landau, and ARRM team NASA/JPL-CalTech © 2014 California Institute of Technology. Government sponsorship acknowledged. Distant Retrograde Orbits Works for Earth, Moon, Mars, Phobos, Deimos etc… very stable orbits Other Lunar Storage Orbit Options • Lagrange Points – Earth-Moon L1/L2 • Unstable; this instability enables many interesting low-energy transfers but vehicles require active station keeping to stay in vicinity of L1/L2 – Earth-Moon L4/L5 • Some orbits in this region is may be stable, but are difficult for MPCV to reach • Lunar Weakly Captured Orbits – These are the transition from high lunar orbits to Lagrange point orbits – They are a new and less well understood class of orbits that could be long term stable and could be easier for the MPCV to reach than DROs – More study is needed to determine if these are good options • Intermittent Capture – Weakly captured Earth orbit, escapes and is then recaptured a year later • Earth Orbit with Lunar Gravity Assists – Many options with Earth-Moon gravity assist tours Backflip Orbits • A backflip orbit is two flybys half a rev apart • Could be done with the Moon, Earth or Mars. Backflip orbit • Lunar backflips are nice plane because they could be used to “catch and release” asteroids • Earth backflips are nice orbits in which to construct things out of asteroids before sending them on to places like Earth- Earth or Moon orbit plane Mars cyclers 4 Example Mars Cyclers Two-Synodic-Period Cycler Three-Synodic-Period Cycler Possibly Ballistic Chen, et al., “Powered Earth-Mars Cycler with Three Synodic-Period Repeat Time,” Journal of Spacecraft and Rockets, Sept.-Oct. -
Global Exploration Roadmap
The Global Exploration Roadmap January 2018 What is New in The Global Exploration Roadmap? This new edition of the Global Exploration robotic space exploration. Refinements in important role in sustainable human space Roadmap reaffirms the interest of 14 space this edition include: exploration. Initially, it supports human and agencies to expand human presence into the robotic lunar exploration in a manner which Solar System, with the surface of Mars as • A summary of the benefits stemming from creates opportunities for multiple sectors to a common driving goal. It reflects a coordi- space exploration. Numerous benefits will advance key goals. nated international effort to prepare for space come from this exciting endeavour. It is • The recognition of the growing private exploration missions beginning with the Inter- important that mission objectives reflect this sector interest in space exploration. national Space Station (ISS) and continuing priority when planning exploration missions. Interest from the private sector is already to the lunar vicinity, the lunar surface, then • The important role of science and knowl- transforming the future of low Earth orbit, on to Mars. The expanded group of agencies edge gain. Open interaction with the creating new opportunities as space agen- demonstrates the growing interest in space international science community helped cies look to expand human presence into exploration and the importance of coopera- identify specific scientific opportunities the Solar System. Growing capability and tion to realise individual and common goals created by the presence of humans and interest from the private sector indicate and objectives. their infrastructure as they explore the Solar a future for collaboration not only among System. -
Planetary Defence Activities Beyond NASA and ESA
Planetary Defence Activities Beyond NASA and ESA Brent W. Barbee 1. Introduction The collision of a significant asteroid or comet with Earth represents a singular natural disaster for a myriad of reasons, including: its extraterrestrial origin; the fact that it is perhaps the only natural disaster that is preventable in many cases, given sufficient preparation and warning; its scope, which ranges from damaging a city to an extinction-level event; and the duality of asteroids and comets themselves---they are grave potential threats, but are also tantalising scientific clues to our ancient past and resources with which we may one day build a prosperous spacefaring future. Accordingly, the problems of developing the means to interact with asteroids and comets for purposes of defence, scientific study, exploration, and resource utilisation have grown in importance over the past several decades. Since the 1980s, more and more asteroids and comets (especially the former) have been discovered, radically changing our picture of the solar system. At the beginning of the year 1980, approximately 9,000 asteroids were known to exist. By the beginning of 2001, that number had risen to approximately 125,000 thanks to the Earth-based telescopic survey efforts of the era, particularly the emergence of modern automated telescopic search systems, pioneered by the Massachusetts Institute of Technology’s (MIT’s) LINEAR system in the mid-to-late 1990s.1 Today, in late 2019, about 840,000 asteroids have been discovered,2 with more and more being found every week, month, and year. Of those, approximately 21,400 are categorised as near-Earth asteroids (NEAs), 2,000 of which are categorised as Potentially Hazardous Asteroids (PHAs)3 and 2,749 of which are categorised as potentially accessible.4 The hazards posed to us by asteroids affect people everywhere around the world. -
Low-Excess Speed Triple Cyclers of Venus, Earth, and Mars
AAS 17-577 LOW EXCESS SPEED TRIPLE CYCLERS OF VENUS, EARTH, AND MARS Drew Ryan Jones,∗ Sonia Hernandez,∗ and Mark Jesick∗ Ballistic cycler trajectories which repeatedly encounter Earth and Mars may be in- valuable to a future transportation architecture ferrying humans to and from Mars. Such trajectories which also involve at least one flyby of Venus are computed here for the first time. The so-called triple cyclers are constructed to exhibit low excess speed on Earth-Mars and Mars-Earth transit legs, and thereby reduce the cost of hyperbolic rendezvous. Thousands of previously undocumented two synodic pe- riod Earth-Mars-Venus triple cyclers are discovered. Many solutions are identified with average transit leg excess speed below 5 km/sec, independent of encounter epoch. The energy characteristics are lower than previously documented cyclers not involving Venus, but the repeat periods are generally longer. NOMENCLATURE ∆tH Earth-Mars Hohmann transfer flight time, days δ Hyperbolic flyby turning angle, degrees R;^ S;^ T^ B-plane unit vectors B B-plane vector, km µ Gravitational parameter, km3/sec2 θB B-plane angle between B and T^, degrees rp Periapsis radius, km T Cycler repeat period, days t0 Cycle starting epoch ∗ t0 Earth-Mars Hohmann transfer epoch tf Cycle ending epoch Tsyn Venus-Earth-Mars synodic period, days v1 Hyperbolic excess speed, km/sec INTRODUCTION Trajectories are computed which ballistically and periodically cycle between flybys of Venus, Earth, and Mars. Using only gravity assists, a cycling vehicle returns to the starting body after a flight time commensurate with the celestial bodies’ orbital periods, thereby permitting indefinite repetition. -
Martian Outpost the Challenges of Establishing a Human Settlement on Mars Erik Seedhouse
Martian Outpost The Challenges of Establishing a Human Settlement on Mars Erik Seedhouse Martian Outpost The Challenges of Establishing a Human Settlement on Mars Springer Published in association with ~ '· i €I Praxis Publishing PR i ~ . i •", . ~ Chichester, UK Dr Erik Seedhouse, F.B.I.S., As.M.A. Milton Ontario Canada SPRINGER±PRAXIS BOOKS IN SPACE EXPLORATION SUBJECT ADVISORY EDITOR: John Mason M.B.E., B.Sc., M.Sc., Ph.D. ISBN 978-0-387-98190-1 Springer Berlin Heidelberg New York Springer is a part of Springer Science + Business Media (springer.com) Library of Congress Control Number: 2009921645 Apart from any fair dealing for the purposes of research or private study, or criticism or review, as permitted under the Copyright, Designs and Patents Act 1988, this publication may only be reproduced, stored or transmitted, in any form or by any means, with the prior permission in writing of the publishers, or in the case of reprographic reproduction in accordance with the terms of licences issued by the Copyright Licensing Agency. Enquiries concerning reproduction outside those terms should be sent to the publishers. # Copyright, 2009 Praxis Publishing Ltd. The use of general descriptive names, registered names, trademarks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. Cover design: Jim Wilkie Copy editor: Dr John Mason Typesetting: BookEns Ltd, Royston, Herts., UK Printed in Germany on acid-free paper Contents Preface ..................................................... xiii Acknowledgments................................................xv About the author .............................................. -
ASTEROID MINING and IN-SITU RESOURCE UTILIZATION A. A. Mardon1 and G
82nd Annual Meeting of The Meteoritical Society 2019 (LPI Contrib. No. 2157) 6189.pdf ASTEROID MINING AND IN-SITU RESOURCE UTILIZATION A. A. Mardon1 and G. Zhou2, 1University of Alberta, 2George Washington University. Introduction: Like many space exploration missions, cost is a determining factor. Transportation alone imposes a cost of $10,000 per kilogram for the entire mission making it simply not profitable or attractive to potential investors. A poten- tial near-instantaneous solution would be to develop an asteroid mining economy developing of a human-commercial market. It is suggested that this scenario will create the economic and technological opportunities not available today. Fu- ture manned missions would require the use of native material and energy on celestial objects to support future human and robotic explorations. The process of collecting and processing usable native material is known as in-situ resource utiliza- tion (ISRU). Currently, space travelling requires missions to carry life necessities such as air, food, water and habitable volume and shielding needed to sustain crew trips from Earth to interplanetary destinations. [1] The possibility of a mis- sion depends on the deduced market value from commercial sale of the product. Engineering choices are identified; a ma- trix of mineralogy, product and process choices can be developed. [2] One major consideration in the process of obtaining energy and life supporting materials from the lunar surface is the identification and excavation of raw material. [3] Lunar soil is produced primarily by meteorite impacts on the surface. This process caused for mineral fragmentation with com- position consisting of miscellaneous glasses, agglutinates and basaltic and brecciated lithic fragments. -
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] -
16. Ice in the Martian Regolith
16. ICE IN THE MARTIAN REGOLITH S. W. SQUYRES Cornell University S. M. CLIFFORD Lunar and Planetary Institute R. O. KUZMIN V.I. Vernadsky Institute J. R. ZIMBELMAN Smithsonian Institution and F. M. COSTARD Laboratoire de Geographie Physique Geologic evidence indicates that the Martian surface has been substantially modified by the action of liquid water, and that much of that water still resides beneath the surface as ground ice. The pore volume of the Martian regolith is substantial, and a large amount of this volume can be expected to be at tem- peratures cold enough for ice to be present. Calculations of the thermodynamic stability of ground ice on Mars suggest that it can exist very close to the surface at high latitudes, but can persist only at substantial depths near the equator. Impact craters with distinctive lobale ejecta deposits are common on Mars. These rampart craters apparently owe their morphology to fluidhation of sub- surface materials, perhaps by the melting of ground ice, during impact events. If this interpretation is correct, then the size frequency distribution of rampart 523 524 S. W. SQUYRES ET AL. craters is broadly consistent with the depth distribution of ice inferred from stability calculations. A variety of observed Martian landforms can be attrib- uted to creep of the Martian regolith abetted by deformation of ground ice. Global mapping of creep features also supports the idea that ice is present in near-surface materials at latitudes higher than ± 30°, and suggests that ice is largely absent from such materials at lower latitudes. Other morphologic fea- tures on Mars that may result from the present or former existence of ground ice include chaotic terrain, thermokarst and patterned ground. -
Technology, Innovation & Engineering Committee Report NASA Advisory
National Aeronautics and Space Administration Technology, Innovation & Engineering Committee Report NASA Advisory Council Presented by: Dr. Bill Ballhaus, Chair December 2, 2015 www.nasa.gov/spacetech TI&E Committee Meeting Attendees November 10, 2015 • Dr. William Ballhaus, Chair • Mr. Gordon Eichhorst, Aperios Partners • Mr. Michael Johns, Southern Research Institute (virtual) • Dr. Matt Mountain, Association of Universities for Research in Astronomy • Mr. David Neyland, Consultant • Mr. Jim Oschmann, Ball Aerospace & Technologies Corp. • Dr. Mary Ellen Weber, STELLAR Strategies, LLC 2 TI&E Committee Meeting Presentations November 10, 2015 • Space Technology Mission Directorate Update – Mr. Stephen Jurczyk, Associate Administrator, STMD • Technology Risk/Challenges Matrix for Humans to Mars and Discussion – Mr. Jason Crusan, Director, Advanced Exploration Systems, HEOMD – Mr. Jim Reuter, Deputy AA for Programs, STMD – Mr. William Gerstenmaier, AA, HEOMD • Chief Technologist Update – Dr. David Miller, NASA Chief Technologist • Agency Technical Capability Assessment Outcomes – Mr. Ralph Roe, NASA Chief Engineer 3 Elements of the Journey to Mars 2010 2020 Now Transition Decade 2030 LEGEND First Human Mars Missions Exploration Human LEO Transition & Cis‐Lunar Habitat Cross-Cutting Long duration human health & habitation build‐up including validation for Mars transit distances (Exploration/Technology/Scie nce) Mars Robotic Precursors Science Identify resources for ISRU, demonstrate round trip surface‐to‐surface capability Asteroid Redirect Mission Human operations in deep space Orion Enabling Crew Operations in Deep Space Space Launch System Traveling beyond low Earth orbit Commercial Cargo and Crew US companies provide affordable access to low earth orbit International Space Station Mastering Long duration stays in space Mars Exploration Program MRO, Curiosity, MAVEN, InSight, Mars 2020. -
Surface Residence Times of Regolith on the Lunar Maria
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1652.pdf 1 1 SURFACE RESIDENCE TIMES OF REGOLITH ON THE LUNAR MARIA. P. O’Brien and S. Byrne , 1 L unar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721 ([email protected]) Introduction: The surfaces of airless bodies like Our model simulates mare-like surfaces evolving the Moon undergo microscopic chemical changes as a over time from flat surfaces to cratered landscapes. result of energetic processes operating in the space Impacts are randomly sampled from the present-day environment, collectively known as space weathering lunar impact flux [5] and the global population of [1,2]. Despite returned lunar soil samples, the rate of secondary craters produced by these impacts is space weathering on the Moon is not well understood. generated following empirical observations of The amount of chemical weathering incurred in the secondary production on airless bodies [6,7]. At each lunar regolith depends critically on the rate at which timestep, we compute the downslope flux of regolith regolith is excavated, transported, and buried by by solving the 2D diffusion equation [8]. The rate of macroscopic impact processes. These physical diffusion is calibrated by matching the average processes control how long regolith spends on the roughness of the model landscapes to the observed surface where it is exposed to the space environment. roughness of the lunar maria, as measured by the We have developed a Monte Carlo model that median bidirectional slope at 4 m baselines [9]. Figure simulates the evolution of lunar maria landscapes 1 shows how model surfaces subject to these physical under topographic relief-creation from impact cratering processes become rougher and more heavily-cratered and relief-reduction from micrometeorite gardening over time. -
NASA Spacecraft Nears Encounter with Dwarf Planet Ceres 4 March 2015
NASA spacecraft nears encounter with dwarf planet Ceres 4 March 2015 of 590 miles (950 kilometers), makes a full rotation every nine hours, and NASA is hoping for a wealth of data once the spacecraft's orbit begins. "Dawn is about to make history," said Robert Mase, project manager for the Dawn mission at NASA JPL in Pasadena, California. "Our team is ready and eager to find out what Ceres has in store for us." Experts will be looking for signs of geologic activity, via changes in these bright spots, or other features on Ceres' surface over time. The latest images came from Dawn when it was 25,000 miles (40,000 kilometers) away on February 25. This image was taken by NASA's Dawn spacecraft of dwarf planet Ceres on February 19, 2015 from a The celestial body was first spotted by Sicilian distance of nearly 29,000 miles astronomer Father Giuseppe Piazzi in 1801. "Ceres was initially classified as a planet and later called an asteroid. In recognition of its planet-like A NASA spacecraft called Dawn is about to qualities, Ceres was designated a dwarf planet in become the first mission to orbit a dwarf planet 2006, along with Pluto and Eris," NASA said. when it slips into orbit Friday around Ceres, the most massive body in the asteroid belt. Ceres is named after the Roman goddess of agriculture and harvests. The mission aims to shed light on the origins of the solar system 4.5 billion years ago, from its "rough The spacecraft on its way to circle it was launched and tumble environment of the main asteroid belt in September 2007.