The Technical and Economic Feasibility of Mining the Near-Earth Asteroids
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1986 DA and 1986 EB: IRON OBJECTS in NEAR-Eakm ORBITS; J.C
LPSC XVIII 349 1986 DA AND 1986 EB: IRON OBJECTS IN NEAR-EAKm ORBITS; J.C. Gra- die, Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii, Bonolalu, HI 96822 and E.F. Tede sco, Jet Propulsion Laboratory, Pasadena, CA 91109. The estimated 1,500 asteroids, with diameters larger than a few hun- dred meters, which cross or closely approach the Earth' s orbit are divided into three orbital classes: the Aten asteroids with semi-maj or axes less than 1 AU and which cross the Earth's orbit near aphelia, the Apollo asteroids with semi-major axes greater than or equal to 1 AU and with per- ihelia greater than 1.17 AU, and the Amor asteroids with perihelia between 1.17 and 1.3 AU (1). These asteroids which have orbits stable against col- 8 lision with or ejection by a planet on the order of lo7 to 10 years must be derived from either extinct cometary naclei (2) or the asteroid belt (C f. 1). These near-Earth asteroids are important for several diverse reasons: they represent a group of obj ect s from which at least some of the meteor- ites arc derived, they may harbor extinct cometary nuclei thought to con- tain some of the most primitive and, perhaps, pristine material in the solar system, occasionally collide with the Earth, and are among the most accessible objects in the solar system. Study of the physical properties of the Earth-approaching asteroids is constrained by the generally long time between close approaches and poorly known orbits. -
Ice& Stone 2020
Ice & Stone 2020 WEEK 34: AUGUST 16-22 Presented by The Earthrise Institute # 34 Authored by Alan Hale This week in history AUGUST 16 17 18 19 20 21 22 AUGUST 16, 1898: DeLisle Stewart at Harvard College Observatory’s Boyden Station in Arequipa, Peru, takes photographs on which Saturn’s outer moon Phoebe is discovered, although the images of Phoebe were not noticed until the following March by William Pickering. Phoebe was the first planetary moon to be discovered via photography, and it and other small planetary moons are discussed in last week’s “Special Topics” presentation. AUGUST 16, 2009: A team of scientists led by Jamie Elsila of the Goddard Space Flight Center in Maryland announces that they have detected the presence of the amino acid glycine in coma samples of Comet 81P/ Wild 2 that were returned to Earth by the Stardust mission 3½ years earlier. Glycine is utilized by life here on Earth, and the presence of it and other organic substances in the solar system’s “small bodies” is discussed in this week’s “Special Topics” presentation. AUGUST 16 17 18 19 20 21 22 AUGUST 17, 1877: Asaph Hall at the U.S. Naval Observatory in Washington, D.C. discovers Mars’ larger, inner moon, Phobos. Mars’ two moons, and the various small moons of the outer planets, are the subject of last week’s “Special Topics” presentation. AUGUST 17, 1989: In its monthly batch of Minor Planet Circulars (MPCs), the IAU’s Minor Planet Center issues MPC 14938, which formally numbers asteroid (4151), later named “Alanhale.” I have used this asteroid as an illustrative example throughout “Ice and Stone 2020” “Special Topics” presentations. -
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. -
NASA Chat: Asteroid 1998 QE2 to Sail Past Earth Expert Dr. Bill Cooke May 30, 2013 ______
NASA Chat: Asteroid 1998 QE2 to Sail Past Earth Expert Dr. Bill Cooke May 30, 2013 _____________________________________________________________________________________ Moderator_Brooke: Welcome everyone! We're just about to start the chat, so please go ahead and send in your questions. Thanks for being here -- now let's talk asteroids! RSEW: Hello Bill_Cooke: We're here! Do you have a question? Moderator_Brooke: All right, here we go...Bill, over to you. tyler_hussey : I was wondering if people in New Hampshire will be able to view this asteroid pass by, and if so, what is the length it will be visible, what direction, and how close to the horizon? Bill_Cooke; Hi Tyler. You need a telescope to see the QE2 asteroid, and of course, it needs to be dark. It's visible there in N.H. with a small telescope about 10:30 p.m. local time. It will be in the constellation Hydra and be about eleventh magnitude. tyler_hussey: I was wondering if people in New Hampshire will be able to view this asteroid pass by, and if so, what is the length it will be visible, what direction, and how close to the horizon? Bill_Cooke: Unless you are Asia or Europe, you will not be able to see the asteroid at close approach. However, you can see it tonight around 10:30 pm local time with a small telescope. It will be in the constellation of Hydra. Moderator_Brooke: You can also find more information about QE2 at this link: http://www.nasa.gov/mission_pages/asteroids/news/asteroid20130530.html guest100: where did this asteroid come from Bill_Cooke: The asteroid 1998 QE2 is an amor asteroid which means it approaches Earth from the outside. -
Physical Properties of Near-Earth Asteroids
Planet. Space Sci., Vol. 46, No. 1, pp. 47-74, 1998 Pergamon N~I1998 Elsevier Science Ltd All rights reserved. Printed in Great Britain 00324633/98 $19.00+0.00 PII: SOO32-0633(97)00132-3 Physical properties of near-Earth asteroids D. F. Lupishko’ and M. Di Martino’ ’ Astronomical Observatory of Kharkov State University, Sumskaya str. 35, Kharkov 310022, Ukraine ‘Osservatorio Astronomic0 di Torino, I-10025 Pino Torinese (TO), Italy Received 5 February 1997; accepted 20 June 1997 rather small objects, usually of the order of a few kilo- metres or less. MBAs of such sizes are generally not access- ible to ground-based observations. Therefore, when NEAs approach the Earth (at distances which can be as small as 0.01-0.02 AU and sometimes less) they give a unique chance to study objects of such small sizes. Some of them possibly represent primordial matter, which has preserved a record of the earliest stages of the Solar System evolution, while the majority are fragments coming from catastrophic collisions that occurred in the asteroid main- belt and could provide “a look” at the interior of their much larger parent bodies. Therefore, NEAs are objects of special interest for sev- eral reasons. First, from the point of view of fundamental science, the problems raised by their origin in planet- crossing orbits, their life-time, their possible genetic relations with comets and meteorites, etc. are closely connected with the solution of the major problem of “We are now on the threshold of a new era of asteroid planetary science of the origin and evolution of the Solar studies” System. -
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. -
Origin and Evolution of Trojan Asteroids 725
Marzari et al.: Origin and Evolution of Trojan Asteroids 725 Origin and Evolution of Trojan Asteroids F. Marzari University of Padova, Italy H. Scholl Observatoire de Nice, France C. Murray University of London, England C. Lagerkvist Uppsala Astronomical Observatory, Sweden The regions around the L4 and L5 Lagrangian points of Jupiter are populated by two large swarms of asteroids called the Trojans. They may be as numerous as the main-belt asteroids and their dynamics is peculiar, involving a 1:1 resonance with Jupiter. Their origin probably dates back to the formation of Jupiter: the Trojan precursors were planetesimals orbiting close to the growing planet. Different mechanisms, including the mass growth of Jupiter, collisional diffusion, and gas drag friction, contributed to the capture of planetesimals in stable Trojan orbits before the final dispersal. The subsequent evolution of Trojan asteroids is the outcome of the joint action of different physical processes involving dynamical diffusion and excitation and collisional evolution. As a result, the present population is possibly different in both orbital and size distribution from the primordial one. No other significant population of Trojan aster- oids have been found so far around other planets, apart from six Trojans of Mars, whose origin and evolution are probably very different from the Trojans of Jupiter. 1. INTRODUCTION originate from the collisional disruption and subsequent reaccumulation of larger primordial bodies. As of May 2001, about 1000 asteroids had been classi- A basic understanding of why asteroids can cluster in fied as Jupiter Trojans (http://cfa-www.harvard.edu/cfa/ps/ the orbit of Jupiter was developed more than a century lists/JupiterTrojans.html), some of which had only been ob- before the first Trojan asteroid was discovered. -
Jjmonl 1710.Pmd
alactic Observer John J. McCarthy Observatory G Volume 10, No. 10 October 2017 The Last Waltz Cassini’s final mission and dance of death with Saturn more on page 4 and 20 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue INTERNATIONAL OBSERVE THE MOON NIGHT ...................... 4 SOLAR ACTIVITY ........................................................... 19 MONTE APENNINES AND APOLLO 15 .................................. 5 COMMONLY USED TERMS ............................................... 19 FAREWELL TO RING WORLD ............................................ 5 FRONT PAGE ............................................................... -
Exploreneos. I. DESCRIPTION and FIRST RESULTS from the WARM SPITZER NEAR-EARTH OBJECT SURVEY
The Astronomical Journal, 140:770–784, 2010 September doi:10.1088/0004-6256/140/3/770 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. EXPLORENEOs. I. DESCRIPTION AND FIRST RESULTS FROM THE WARM SPITZER NEAR-EARTH OBJECT SURVEY D. E. Trilling1, M. Mueller2,J.L.Hora3, A. W. Harris4, B. Bhattacharya5, W. F. Bottke6, S. Chesley7, M. Delbo2, J. P. Emery8, G. Fazio3, A. Mainzer7, B. Penprase9,H.A.Smith3, T. B. Spahr3, J. A. Stansberry10, and C. A. Thomas1 1 Department of Physics and Astronomy, Northern Arizona University, Flagstaff, AZ 86001, USA; [email protected] 2 Observatoire de la Coteˆ d’Azur, Universite´ de Nice Sophia Antipolis, CNRS, BP 4229, 06304 Nice Cedex 4, France 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-65, Cambridge, MA 02138, USA 4 DLR Institute of Planetary Research, Rutherfordstrasse 2, 12489 Berlin, Germany 5 NASA Herschel Science Center, Caltech, M/S 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA 6 Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA 7 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 8 Department of Earth and Planetary Sciences, University of Tennessee, 1412 Circle Drive, Knoxville, TN 37996, USA 9 Department of Physics and Astronomy, Pomona College, 610 North College Avenue, Claremont, CA 91711, USA 10 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA Received 2009 December 18; accepted 2010 July 6; published 2010 August 9 ABSTRACT We have begun the ExploreNEOs project in which we observe some 700 Near-Earth Objects (NEOs) at 3.6 and 4.5 μm with the Spitzer Space Telescope in its Warm Spitzer mode. -
Robotic Asteroid Prospector
Robotic Asteroid Prospector Marc M. Cohen1 Marc M. Cohen Architect P.C. – Astrotecture™, Palo Alto, CA, USA 94306-3864 Warren W. James2 V Infinity Research LLC. – Altadena, CA, USA Kris Zacny,3 Philip Chu, Jack Craft Honeybee Robotics Spacecraft Mechanisms Corporation – Pasadena, CA, USA This paper presents the results from the nine-month, Phase 1 investigation for the Robotic Asteroid Prospector (RAP). This project investigated several aspects of developing an asteroid mining mission. It conceived a Space Infrastructure Framework that would create a demand for in space-produced resources. The resources identified as potentially feasible in the near-term were water and platinum group metals. The project’s mission design stages spacecraft from an Earth Moon Lagrange (EML) point and returns them to an EML. The spacecraft’s distinguishing design feature is its solar thermal propulsion system (STP) that provides two functions: propulsive thrust and process heat for mining and mineral processing. The preferred propellant is water since this would allow the spacecraft to refuel at an asteroid for its return voyage to Cis- Lunar space thus reducing the mass that must be launched from the EML point. The spacecraft will rendezvous with an asteroid at its pole, match rotation rate, and attach to begin mining operations. The team conducted an experiment in extracting and distilling water from frozen regolith simulant. Nomenclature C-Type = Carbonaceous Asteroid EML = Earth-Moon Lagrange Point ESL = Earth-Sun Lagrange Point IPV = Interplanetary Vehicle M-Type = Metallic Asteroid NEA = Near Earth Asteroid NEO = Near Earth Object PGM = Platinum Group Metal STP = Solar Thermal Propulsion S-Type = Stony Asteroid I. -
Small Meteor Showers Identification with Near-Earth Asteroids
SMALL METEOR SHOWERS INDENTIFICATION WITH NEAR-EARTH ASTEROIDS M.V. Sergienko, M.G. Sokolova, A.O. Andreev, Y.A. Nefedyev Kazan Federal University, Kazan, Russia Results As a result, with a probability of more than 0,6 the following results are obtained. With the orbits similar to k-Cygnids, the asteroids 2001MG1, 2002LV (noted in works by other authors) from the Apollo group and 2002GJ8, 2012QH49, 2010QA5 from the Amor group are marked out. For δ-Cancrids only asteroids from the Apollo group are marked out: northern NCC – 2212 Hephaistos 1978SB, 2014RS17, 2011SR12; southern SCC - 2015PC, 1991AQ, 2006BF56. For the general δ-Cancrids complex 2006BF56, 2014RS17, 1991AQ, 2003RW11, 2001YB5 are marked out. For Virginids only asteroids from the Apollo group are marked out: 2006UF17, 2008VL14, 2010VF. Asteroids in groups for each shower have been identified with a probability of less than 0,2. The initial base of asteroids contained 17800 orbits. The statistics for the showers is as follows: k-Cygnids – 700, δ-Cancrids (NCC, SCC branches) – 170, Virginids – 12. Analysis of the modern NEOs orbits shows that the majority of them are formed in the main asteroid belt located between the orbits of Mars and Jupiter [1]. As we see, the orbits of the marked-out asteroids are elongated and comet-like. The size of 153311(2001 Introduction MG1) and 385343(2002 LV) asteroids are also typical of comet nuclei, while 2014 RS17 and 2006 BF56 Currently, Near-Earth Objects (NEO), small bodies of the Solar asteroids having small size are probably the products of larger body disintegration. For newly discovered system including asteroids and comets with elongated orbits asteroids, orbit elements are reliably determined, but other parameters, such as taxonomic index (TI) and diameter (D), are determined less reliably or unknown. -
Asteroid Regolith Weathering: a Large-Scale Observational Investigation
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 5-2019 Asteroid Regolith Weathering: A Large-Scale Observational Investigation Eric Michael MacLennan University of Tennessee, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Recommended Citation MacLennan, Eric Michael, "Asteroid Regolith Weathering: A Large-Scale Observational Investigation. " PhD diss., University of Tennessee, 2019. https://trace.tennessee.edu/utk_graddiss/5467 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Eric Michael MacLennan entitled "Asteroid Regolith Weathering: A Large-Scale Observational Investigation." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Joshua P. Emery, Major Professor We have read this dissertation and recommend its acceptance: Jeffrey E. Moersch, Harry Y. McSween Jr., Liem T. Tran Accepted for the Council: Dixie L. Thompson Vice Provost and Dean of the Graduate School (Original signatures are on file with official studentecor r ds.) Asteroid Regolith Weathering: A Large-Scale Observational Investigation A Dissertation Presented for the Doctor of Philosophy Degree The University of Tennessee, Knoxville Eric Michael MacLennan May 2019 © by Eric Michael MacLennan, 2019 All Rights Reserved.