DOCSLIB.ORG

Plymouth Rock: an Early Human Asteroid Mission Using Orion

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Plymouth Rock: an Early Human Asteroid Mission Using Orion Plymouth Rock: An Early Human Asteroid Mission Using Orion Presented to the Small Bodies Assessment Group November 2009 Lockheed Martin Proprietary Josh Hopkins, Adam Dissel Information Lockheed Martin Space Systems Company1 Study Background • Lockheed Martin began investigating asteroid missions using Orion in 2007 – Our study focused on how to perform an asteroid mission as a complement to the baseline Constellation Program ’s lunar mission plans. Some details may change if NASA ’s baseline changes but the results are broadly applicable. • The results presented here are based on internally funded research, and do not imply endorsement by NASA or any change in program plans for the Orion crew exploration vehicle or the Constellation Program 2 A New Destination for Human Spaceflight • In the past ten years, astronomers have discovered dozens of asteroids in Earth -like orbits – Discoveries are continuing and accelerating • Some of these new asteroids are accessible with lunar -class exploration spacecraft and launch vehicles, rather than Mars -class systems • These recent discoveries are so new that the implications for human spaceflight of are still being determined and are not incorporated in prior spaceflight planning – Asteroids used to be the “beyond ” in “Moon, Mars and Beyond, ” but now they could be “Moon, Mars and Between ” or perhaps even “Before ” 3 Asteroid Orbits • Main Belt Asteroids (~450,000 known) Most asteroids, like Ceres , orbit far beyond Mars and are not yet accessible for human missions Ceres 4 Earth’s Known Neighbors, circa 1990 Era of Space Exploration Initiative, Stafford & Augustine Reports 0.125 (No Known Orbital Neighbors) 0.1 0.075 Eccentricity 0.05 Asteroid Inclinations i < 1 Region of 0.025 1< i < 2 Accessible Orbits 2< i < 3 3 < i < 5 EARTH & MOON 0 Mars at 0.9 0.95 1 1.05 1.1 1.5 A.U. Asteroids known as of year-end 1990 Glyph size proportional to asteroid size (5-75 m) Semi-Major Axis (A.U.) (Earth not to scale) Image of Earth and Moon from Deep Impact, courtesy NASA 5 Earth’s Known Neighbors, circa 2003 Columbia Accident, Vision for Space Exploration Formulated 0.125 2000 LG6 1999 AO10 0.1 2001 QJ142 2001 GP2 0.075 2000 SG344 Eccentricity 0.05 1991 VG Asteroid Inclinations i < 1 Region of 0.025 1< i < 2 Accessible Orbits 2< i < 3 3 < i < 5 EARTH & MOON 0 Mars at 0.9 0.95 1 1.05 1.1 1.5 A.U. Asteroids known as of autumn 2003 Glyph size proportional to asteroid size (5-75 m) Semi-Major Axis (A.U.) (Earth not to scale) Image of Earth and Moon from Deep Impact, courtesy NASA 6 Earth’s Known Neighbors, July 2009 Era of Second Augustine Committee 0.125 2008 DL4 2004 QA22 2007 YF 2003 WP25 2000 LG6 2007 DD 1999 AO10 2006 BZ147 2008 JL24 0.1 2007 VU6 2008 KT 2001 QJ142 2006 JY26 2001 GP2 2008 EA9 0.075 2008 HU4 2000 SG344 2008 UA202 2007 UN12 Eccentricity 0.05 2006 QQ56 1991 VG Asteroid Inclinations 2009 BD i < 1 Region of 2006 RH120 0.025 1< i < 2 Accessible Orbits 2< i < 3 2003 YN107 3 < i < 5 EARTH & MOON 0 Mars at 0.9 0.95 1 1.05 1.1 1.5 A.U. Asteroids known as of summer 2009 Glyph size proportional to asteroid size (5-75 m) Semi-Major Axis (A.U.) (Earth not to scale) Image of Earth and Moon from Deep Impact, courtesy NASA 7 WhatWhat areare thesethese objects?objects? • Small asteroids (5 -70 meter sized) in Earth -like orbits – The smallest are mostly harmless, but the largest are similar in size to the impactors which caused the Tunguska Event and Barringer Crater • Origin and composition of these objects are uncertain – Small size makes them hard to study telescopically – Arrived in these orbits within the last 100,000 years – Mostly shattered remnants of larger asteroids in the main belt which migrated to closer orbits – A few might be defunct spacecraft, burned out comets, or even ejecta from recent lunar craters – Spin rates are undetermined for most of these objects, but the few known spin rates are very fast (a few minutes per rev) • Likely to be monolithic rather than ‘rubble piles ’ 8 WhyWhy ExploreExplore anan Asteroid?Asteroid? • Knowledge – Study formation and history of our solar system – Correlate asteroid families to meteorite samples • Security – Enable deflection of future hazardous impactors by understanding structure, composition, and how to operate around small asteroid s • Wealth – Evaluate viability of asteroid resources for human expansion in space • National Pride – Decisively re -establish American preeminence in space – Reduce the ‘exploration gap ’ before the next human lunar landing • Training – If a lunar mission precursor: Demonstrate lunar launch profile, LEO rendezvous, and Orion reentry at lunar -like entry speeds – As a Mars mission precursor: Learn to fly human missions in deep space, with speed of light lag, radiation risk, and no resupply or rescue. Asteroids are shorter, simpler practice for Mars mission s. 9 How Can We Explore the Asteroids? • Favorable orbital alignments occur only a few times per decade, so it may not make sense to design a new human spacecraft just for asteroid missions • Orion can b e used to launch and return astronauts, but these missions need an additional space craft element to provide more deep -space propulsion, living space, food, water, and oxygen • A second, modified Orion can be the additional elem ent , rather than investing in new spacecraft – Provides capability and substant ial redundancy at low cost and within schedule timeframe without a new program start – Altair lunar lander may be an alternative depending on budget and design details (e.g. if boiloff rate < 0.25%/day) 10 MissionMission ConceptConcept UtilizingUtilizing DualDual OrionsOrions Asteroid Exploration (~5 days) Asteroid Arrival Trans Earth Maneuver Injection Outbound Return LEO Earth Transfer (~ 3 months) Rendezvous Departure (~ 3 months) LEO Re-entry Ares V Launch Ares I Launch Supplemental Primary Orion Orion + EDS (Manned) Recovery (Unmanned) • Plymouth Rock asteroid mission architecture mimics baseline Constellation lunar mission profile except: – Supplemental Orion replaces Altair lunar lander – Asteroid target replaces Moon – Crew of two rather than four due to limited volume and supplies 11 Asteroid Exploration Operations • We can ’t ‘land ’ or ‘moonwalk ’ on an ast eroid this small. Instead, spacewalk next to it, somewhat analogous to satellite servicing missions of the 1980s. • First, rendezvous with the asteroid and observe from several km away for basic mapping and to look for co -orbiting debris • Then, approach closer and station keep ~100 meters away – Keeping the spacecraft some distance from the asteroid rather than landing simplifies power, communications, thermal, GNC , etc. • Depress urize one Orion crew module to perform s pacewalks • Use an MMU -like spacesuit propulsion system to approach an asteroid and collect samples • Small asteroids likely have negative surface gravity due to rapid rotation periods – Makes EVA operations challenging – Probably means these asteroids don ’t have loose gravel or regolith that would be easy to sample • Many open ques tions are still to be resolved regarding how to perform EVAs near asteroids 12 AsteroidAsteroid MissionMission OpportunitiesOpportunities 20152015 --20302030 UsingUsing DualDual OrionOrion oror OrionOrion ++ AltairAltair Mission Duration for Various Propulsion Capabilities Prime Orion Prime Orion 25% More Asteroid Launch Date Diameter Orion + Altair Offloaded for Full Prop Prop in Each (estimate) Ares 1 Load Orion 2008 HU4 Apr 2016 7-10 m Not feasible 190 days 115 days 95 days 1991 VG Jul 2017 6-9 m 230 days 220 days 190 days 175 days 2008 EA9 Nov 2019 8-12 m 205 days 190 days 175 days 165 days 2007 UN12 Jul 2020 5-8 m 235 days 230 days 215 days 210 days 1999 AO10 Aug 2025 50-70 m Not feasible Not feasible Not feasible Not feasible 2008 JL24 Feb 2026 4-5 m Not feasible Not feasible Not feasible 205 days 2006 RH120 Jun 2028 4-5 m 165 days 145 days 115 days 95 days 2000 SG344 Jul 2029 30-45 m 155 days 145 days 130 days 125 days • Six months appears to be the upper limit of feasible mission dur ations using dual Orion • Longer missions are difficult due to radiation, limited habitabl e volume, life support consumables, etc. • Shorter missions are better • Repeat opportunities with a specific asteroid are usually decade s apart • At the current asteroid discovery rate, the number of known miss ion opportunities in this time frame may double by 2015 13 2019 Opportunity: 2008 EA9 2019 Opportunity to Asteroid 2008 EA9 Total Mission DV = 4.9 km/s Total 205 Day Mission Duration 2008 EA9 Orbit Return Transfer Landing 106 Days June 7, 2020 Earth Orbit Departure Feb 22, 2020 Launch Arrival Nov 15, 2019 Feb 17, 2020 5 days at NEO Outbound Transfer 94 days 108 Distance in km x Heliocentric-Ecliptic Coordinate System 14 2019 Opportunity: 2008 EA9 Max Distance from Earth 2019 Opportunity to 2008 EA9 = 12.2 million km Total Mission DV = 4.9 km/s = 32 x lunar distance Total 205 Day Mission Duration = 0.08 A.U. Atmospheric Entry = 40 light-seconds Moon Orbit 11.12 km/s Return Transfer Earth Departure 106 Days 3.305 km/s Outbound Transfer 2008 EA9 94 days at Launch Trans-Earth Injection 1.15 km/s Asteroid Arrival Maneuver 2008 EA9 0.44 km/s at Landing Trajectory Tick Marks in 15 Day Increments Geocentric-Ecliptic Coordinate System 15 Initial Feasibility Assessment •• Two Orions together provide just enough habitable volume for two astronauts •• Dual Orions can accommodate additional food, water, and oxygen needed for two people on 180 day missions within volume and mass limits –– The crewed Orion launch is mass constrained by launch performance and the capability of the launch abort system and recovery system.
Load more

Recommended publications
  • Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar End
    N9 Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar end Planetary Laboratory The University of Arizona Our overall scientific goal is to survey the solar system to completion -- that is, to find the various populations and to study their statistics, interrelations, and origins. The practical benefit to SERC is that we are finding Earth-approaching asteroids that are accessible for mining. Our system can detect Earth-approachers In the 1-km size range even when they are far away, and can detect smaller objects when they are moving rapidly past Earth. Until Spacewatch, the size range of 6 - 300 meters in diameter for the near-Earth asteroids was unexplored. This important region represents the transition between the meteorites and the larger observed near-Earth asteroids (Rabinowitz 1992). One of our Spacewatch discoveries, 1991 VG, may be representative of a new orbital class of object. If it is really a natural object, and not man-made, its orbital parameters are closer to those of the Earth than we have seen before; its delta V is the lowest of all objects known thus far (J. S. Lewis, personal communication 1992). We may expect new discoveries as we continue our surveying, with fine-tuning of the techniques. III-12 Introduction The data accumulated in the following tables are the result of continuing observation conducted as a part of the Spacewatch program. T. Gehrels is the Principal Investigator and also one of the three observers, with J.V. Scotti and D.L Rabinowitz, each observing six nights per month. R.S. McMillan has been Co-Principal Investigator of our CCD-scanning since its inception; he coordinates optical, mechanical, and electronic upgrades.
    [Show full text]
  • Asteroid Retrieval Feasibility Study
    Publications 4-2-2012 Asteroid Retrieval Feasibility Study John Brophy California Institute of Technology Fred Culick California Institute of Technology Louis Friedman The Planetary Society Pedro Llanos Embry-Riddle Aeronautical University - Daytona Beach, [email protected] et al. Follow this and additional works at: https://commons.erau.edu/publication Part of the Astrodynamics Commons, Space Vehicles Commons, and the The Sun and the Solar System Commons Scholarly Commons Citation Brophy, J., Culick, F., Friedman, L., Llanos, P., & al., e. (2012). Asteroid Retrieval Feasibility Study. , (). Retrieved from https://commons.erau.edu/publication/893 This Report is brought to you for free and open access by Scholarly Commons. It has been accepted for inclusion in Publications by an authorized administrator of Scholarly Commons. For more information, please contact [email protected]. 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
    [Show full text]
  • An Ongoing Effort to Identify Near-Earth Asteroid Destination
    The Near-Earth Object Human Space Flight Accessible Targets Study: An Ongoing Effort to Identify Near-Earth Asteroid Destinations for Human Explorers Presented to the 2013 IAA Planetary Defense Conference Brent W. Barbee∗, Paul A. Abelly, Daniel R. Adamoz, Cassandra M. Alberding∗, Daniel D. Mazanekx, Lindley N. Johnsonk, Donald K. Yeomans#, Paul W. Chodas#, Alan B. Chamberlin#, Victoria P. Friedensenk NASA/GSFC∗ / NASA/JSCy / Aerospace Consultantz NASA/LaRCx / NASA/HQk / NASA/JPL# April 16th, 2013 Introduction I Near-Earth Objects (NEOs) are asteroids and comets with perihelion distance < 1.3 AU I Small, usually rocky bodies (occasionally metallic) I Sizes range from a few meters to ≈ 35 kilometers I Near-Earth Asteroids (NEAs) are currently candidate destinations for human space flight missions in the mid-2020s th I As of April 4 , 2013, a total of 9736 NEAs have been discovered, and more are being discovered on a continual basis 2 Motivations for NEA Exploration I Solar system science I NEAs are largely unchanged in composition since the early days of the solar system I Asteroids and comets may have delivered water and even the seeds of life to the young Earth I Planetary defense I NEA characterization I NEA proximity operations I In-Situ Resource Utilization I Could manufacture radiation shielding, propellant, and more I Human Exploration I The most ambitious journey of human discovery since Apollo I NEAs as stepping stones to Mars 3 NHATS Background I NASA's Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) (pron.: /næts/) began in September of 2010 under the auspices of the NASA Headquarters Planetary Science Mission Directorate in cooperation with the Advanced Exploration Systems Division of the Human Exploration and Operations Mission Directorate.
    [Show full text]
  • Near Earth Asteroid (NEA) Scout
    https://ntrs.nasa.gov/search.jsp?R=20160007060 2019-08-08T05:23:13+00:00Z Near Earth Asteroid (NEA) Scout Les Johnson NASA MSFC Advance Concepts Office [email protected] Topics • What is a solar sail? • A brief history of solar sailing • NASA’s Near Earth Asteroid Scout mission How does a solar sail work? Solar sails use photon “pressure” or force on thin, lightweight reflective sheet to produce thrust. 3 Topics • What is a solar sail? • A brief history of solar sailing • NASA’s Near Earth Asteroid Scout mission The Planetary Society’s Cosmos-1 (2005) • 100 kg spacecraft • 8 triangular sail blades deployed from a central hub after launch by the inflating of structural tubes. • Sail blades were each 15 m long • Total surface area of 600 square meters • Launched in 2005 from a Russian Volna Rocket from a Russian Delta III submarine in the Barents Sea: The Planetary Society’s Cosmos-1 (2005) • 100 kg spacecraft • 8 triangular sail blades deployed from a central hub after launch by the inflating of structural tubes. • Sail blades were each 15 m long • Total surface area of 600 square meters • Launched in 2005 from a Russian Volna Rocket from a Russian Delta III submarine in the Barents Sea: Rocket Failed NASA Ground Tested Solar Sails in the Mid-2000’s Two 400 square meter sail were autonomously deployed and tested at Plumbrook NanoSail-D Demonstration Solar Sail Mission Description: • 10 m2 sail • Made from tested ground demonstrator hardware NanoSail-D2 Mission (2010) Interplanetary Kite-craft Accelerated by Radiation of the Sun (IKAROS)
    [Show full text]
  • Discovery of Earth's Quasi-Satellite
    Meteoritics & Planetary Science 39, Nr 8, 1251–1255 (2004) Abstract available online at http://meteoritics.org Discovery of Earth’s quasi-satellite Martin CONNORS,1* Christian VEILLET,2 Ramon BRASSER,3 Paul WIEGERT,4 Paul CHODAS,5 Seppo MIKKOLA,6 and Kimmo INNANEN3 1Athabasca University, Athabasca AB, Canada T9S 3A3 2Canada-France-Hawaii Telescope, P. O. Box 1597, Kamuela, Hawaii 96743, USA 3Department of Physics and Astronomy, York University, Toronto, ON M3J 1P3 Canada 4Department of Physics and Astronomy, University of Western Ontario, London, ON N6A 3K7, Canada 5Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109, USA 6Turku University Observatory, Tuorla, FIN-21500 Piikkiö, Finland *Corresponding author. E-mail: [email protected] (Received 18 February 2004; revision accepted 12 July 2004) Abstract–The newly discovered asteroid 2003 YN107 is currently a quasi-satellite of the Earth, making a satellite-like orbit of high inclination with apparent period of one year. The term quasi- satellite is used since these large orbits are not completely closed, but rather perturbed portions of the asteroid’s orbit around the Sun. Due to its extremely Earth-like orbit, this asteroid is influenced by Earth’s gravity to remain within 0.1 AU of the Earth for approximately 10 years (1997 to 2006). Prior to this, it had been on a horseshoe orbit closely following Earth’s orbit for several hundred years. It will re-enter such an orbit, and make one final libration of 123 years, after which it will have a close interaction with the Earth and transition to a circulating orbit.
    [Show full text]
  • 1 ABSTRACT Aside from the Exploration of Mars, the Objects That
    IAC-07-B3.5.06 INTO THE BEYOND: A CREWED MISSION TO A NEAR-EARTH OBJECT David J. Korsmeyer, NASA Ames Research Center, Intelligent Systems Division, Moffett Field, CA, USA, [email protected] Rob R. Landis, NASA Johnson Space Center, Mission Operations Directorate, Houston, TX, USA [email protected] Paul A. Abell, NASA Johnson Space Center, Astromaterials Research & Exploration Science, Houston, TX, USA [email protected] ABSTRACT utility and opportunities for the developing Aside from the exploration of Mars, the Constellation infrastructure, particularly, the objects that most capture our interest for a Ares Launch vehicles and the Orion crewed new human visit are the Near-Earth Objects spacecraft, to be used for missions that were (NEOs). These objects are ideal candidates not directly in the design specifications (aka for deep space operations and explorations as non-lunar missions). The Ares and Orion we extend the human presence out into the systems are designed to launch 4-6 crew to solar system. The notion of a crewed mission the International Space Station (ISS), and to to a NEO was first discussed in the Apollo eventually take 4 crew back to lunar orbit era. The most recent assessment has been where a lunar lander would take the crew to undertaken by the Advanced Projects Office the surface. within NASA’s Constellation Program. This particular study examined the feasibility of The NASA Constellation Program wanted to sending NASA’s new Orion spacecraft (also understand what are some other feasible, referred to as the Crew Exploration Vehicle, high-value uses of the Orion spacecraft and or CEV) to a NEO.
    [Show full text]
  • Asteroid Retrieval Mission Concept – Trailblazing Our Future in Space and Helping to Protect Us from Earth Impactors
    Asteroid Retrieval Mission Concept – Trailblazing Our Future in Space and Helping to Protect Us from Earth Impactors Presented by Dan Mazanek1 Co-authors: John Brophy2 and Gabe Merrill1 1NASA Langley Research Center; 2Jet Propulsion Laboratory April 16, 2013 2013 Planetary Defense Conference Flagstaff, USA Paper No: IAA-PDC13-04-14 1 Background The idea of utilizing asteroidal resources is not new • 1903 – Konstantin Tsiolkovskii included the concept of using asteroids for resources in his most famous publication, The Exploration of Cosmic Space by Means of Reaction Motors • 1977 – NASA’s Dr. Brian O’Leary proposed using mass drivers to move Earth- approaching Apollo and Amor asteroids to Earth’s vicinity • 1997 – Dr. John S. Lewis detailed how we can extract the vast resources available from our solar system in the influential book Mining the Sky: Untold Riches from the Asteroids, Comets, and Planets September 2011 and February 2012 – Asteroid Retrieval Mission (ARM) Study at Caltech’s Keck Institute for Space Studies (KISS) • Examined the feasibility of returning a small (~7 m diameter) near-Earth asteroid (NEA), or part of a large NEA, to cislunar space • Utilize robotic 50 kW-class solar electric propulsion (SEP) vehicle and currently available technologies (40 kW available to the electric propulsion system) • John Brophy (Co-Leader along with Louis Friedman and Fred Culick) and Dan Mazanek were KISS ARM study members 2 Recent Events Recent events have elevated the public’s awareness of the potential of space resources and have
    [Show full text]
  • 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.
    [Show full text]
  • OSIRIS-Rex Goes Asteroid Collecting
    OSIRIS-REx Goes Asteroid Collecting — Scott Messenger, NASA Johnson Space Center OSIRIS-REx is NASA’s third New Frontiers mission, following the New Horizons mission, which completed a flyby of Pluto in 2015, and the Juno mission to orbit Jupiter, which has just begun science operations. The OSIRIS-REx mission’s primary objective is to collect pristine surface samples of a carbonaceous asteroid and return them to Earth for analysis. Carbonaceous asteroids and comets are considered to be L “primitive” bodies that have preserved remnants of the solar system starting materials. By studying them, scientists can learn about the origin and earliest evolution of the solar system. The OSIRIS-REx spacecraft was launched on September 8, 2016, beginning its two- year journey to asteroid 101955 Bennu (formerly designated 1999 RQ36). After more than one year of detailed remote observations, OSIRIS-REx will obtain surface samples and return them to Earth in September 2023. The OSIRIS-REx proposal, led by the late Dr. Michael J. Drake, was selected during the 2011 New Frontiers competition, and is now led by Dr. Dante Lauretta of the University of Arizona. The Pmission name OSIRIS-REx (an acronym for Origins, Spectral Interpretation, Resource Identification, Security, Regolith Explorer) embodies five objectives: (1) Origins: Return and analyze a sample of a carbonaceous asteroid; (2) Spectral Interpretation: Provide ground truth for remote observations of asteroids; (3) Resource Identification: Determine the mineral and chemical makeup of a near-Earth asteroid; (4) Security: Directly measure the non-gravitational force known as the Yarkovsky effect, which changes asteroidal orbits through its Iinteraction with sunlight; and (5) Regolith Explorer: Determine the properties of unconsolidated material that covers the asteroid surface.
    [Show full text]
  • Why Atens Enjoy Enhanced Accessibility for Human Space Flight
    (Preprint) AAS 11-449 WHY ATENS ENJOY ENHANCED ACCESSIBILITY FOR HUMAN SPACE FLIGHT Daniel R. Adamo* and Brent W. Barbee† Near-Earth objects can be grouped into multiple orbit classifications, among them being the Aten group, whose members have orbits crossing Earth's with semi-major axes less than 1 astronomical unit. Atens comprise well under 10% of known near-Earth objects. This is in dramatic contrast to results from recent human space flight near-Earth object accessibility studies, where the most favorable known destinations are typically almost 50% Atens. Geocentric dynamics explain this enhanced Aten accessibility and lead to an understanding of where the most accessible near-Earth objects reside. Without a com- prehensive space-based survey, however, highly accessible Atens will remain largely un- known. INTRODUCTION In the context of human space flight (HSF), the concept of near-Earth object (NEO) accessibility is highly subjective (Reference 1). Whether or not a particular NEO is accessible critically depends on mass, performance, and reliability of interplanetary HSF systems yet to be designed. Such systems would cer- tainly include propulsion and crew life support with adequate shielding from both solar flares and galactic cosmic radiation. Equally critical architecture options are relevant to NEO accessibility. These options are also far from being determined and include the number of launches supporting an HSF mission, together with whether consumables are to be pre-emplaced at the destination. Until the unknowns of HSF to NEOs come into clearer focus, the notion of relative accessibility is of great utility. Imagine a group of NEOs, each with nearly equal HSF merit determined from their individual characteristics relating to crew safety, scientific return, resource utilization, and planetary defense.
    [Show full text]
  • The Population of Near Earth Asteroids in Coorbital Motion with Venus
    ARTICLE IN PRESS YICAR:7986 JID:YICAR AID:7986 /FLA [m5+; v 1.65; Prn:10/08/2006; 14:41] P.1 (1-10) Icarus ••• (••••) •••–••• www.elsevier.com/locate/icarus The population of Near Earth Asteroids in coorbital motion with Venus M.H.M. Morais a,∗, A. Morbidelli b a Grupo de Astrofísica da Universidade de Coimbra, Observatório Astronómico de Coimbra, Santa Clara, 3040 Coimbra, Portugal b Observatoire de la Côte d’Azur, BP 4229, Boulevard de l’Observatoire, Nice Cedex 4, France Received 13 January 2006; revised 10 April 2006 Abstract We estimate the size and orbital distributions of Near Earth Asteroids (NEAs) that are expected to be in the 1:1 mean motion resonance with Venus in a steady state scenario. We predict that the number of such objects with absolute magnitudes H<18 and H<22 is 0.14 ± 0.03 and 3.5 ± 0.7, respectively. We also map the distribution in the sky of these Venus coorbital NEAs and we see that these objects, as the Earth coorbital NEAs studied in a previous paper, are more likely to be found by NEAs search programs that do not simply observe around opposition and that scan large areas of the sky. © 2006 Elsevier Inc. All rights reserved. Keywords: Asteroids, dynamics; Resonances 1. Introduction object with a theory based on the restricted three body problem at high eccentricity and inclination. Christou (2000) performed In Morais and Morbidelli (2002), hereafter referred to as a 0.2 Myr integration of the orbits of NEAs in the vicinity of Paper I, we estimated the population of Near Earth Asteroids the terrestrial planets, namely (3362) Khufu, (10563) Izhdubar, (NEAs) that are in the 1:1 mean motion resonance (i.e., are 1994 TF2 and 1989 VA, showing that the first three could be- coorbital1) with the Earth in a steady state scenario where come coorbitals of the Earth while the fourth could become NEAs are constantly being supplied by the main belt sources coorbital of Venus.
    [Show full text]
  • ANIME: the “ASTEROID NODAL INTERSECTION MULTIPLE ENCOUNTERS” CUBESAT MISSION to EXPLORE NEAR-EARTH ASTEROID DIVERSITY. D. Perna1, M
    52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1106.pdf ANIME: THE “ASTEROID NODAL INTERSECTION MULTIPLE ENCOUNTERS” CUBESAT MISSION TO EXPLORE NEAR-EARTH ASTEROID DIVERSITY. D. Perna1, M. Pajola2, L. Casalino3, S. Ivanovski4, M. Lavagna5, M. Zannoni6, M. Bechini5, A. Capannolo5, A. Colagrossi5, G. Cremonese2, E. Dotto1, A. Lucchetti2, E. Mazzotta Epifani1, J. Prinetto5, E. Simioni2, P. Tortora6 and G. Zanotti5 1INAF – Osservatorio Astronomico di Roma (Italy), [email protected], 2INAF – Osservatorio Astronomico di Padova (Italy), 3DIMEAS – Politecnico di Torino (Italy), 4INAF – Osservatorio Astronomico di Trieste (Italy), 5DAER – Politecnico di Milano (Italy), 6CIRI Aerospace – Università di Bologna (Italy). ANIME in a nutshell: The “Asteroid Nodal positions and velocities. Asteroids 2000 SG344, 2006 Intersection Multiple Encounters” (ANIME) mission HZ51 and 2004 QD14 are selected as ANIME targets concept has been proposed in response to the 2020 due to their pivotal scientific and strategic relevance, Italian Space Agency (ASI) call for ideas for future over a rather large number of suitable alternatives. The CubeSat missions. ANIME aims to explore three near- reference solution (Figure 1) has a total ΔV of 1.05 Earth asteroids (NEAs), selected by virtue of their km/s and a propellant consumption of 1.04 kg (out of peculiar and yet unexplored size and physical regimes, the available 1.5 kg). The ample propellant margin as well as their relevance in terms of planetary guarantees flexibility in terms of: i) departure date protection. Thanks to an optimized trajectory, the changes, ii) strategies for escape from Earth sphere of targets are encountered during their passages through influence (depending on the launch opportunities and their orbital nodes.
    [Show full text]