Research on the Use of Space Resources
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Defending Earth: the Threat from Asteroid and Comet Impact
Defending Earth: The Threat from Asteroid and Comet Impact Version A | 05 September 2009 Mr. A.C. Charania President, Commercial Division | SpaceWorks Engineering, Inc. (SEI) | [email protected] | 1+770.379.8006 Acknowledgments: Multiple slides from Dr. Clark Chapman, Southwest Research Institute Boulder, Colorado, USA, URL: www.boulder.swri.edu/~cchapman 1 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero Source: NASA/JPL/Infrared Telescope Facility 2009 Jupiter Impact Event: 19 July 2009 (1 km Sized Object) 2 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero Source: JPL / NASA Spitzer Space Telescope 95 Light Years Away (Star HD 172555): Moon-Sized Object Impacts Mercury-Sized Object at 10 km/s (5.8+/-0.6 AU Orbit) 3 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero SPACEWORKS 4 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero KEY CUSTOMERS AND PRODUCTS 5 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero DOMAIN OF EXPERTISE: ADVANCED CONCEPTS 6 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero INTRODUCTION 7 Copyright 2009, SpaceWorks Engineering, Inc. (SEI) | www.sei.aero − Asteroid - A relatively small, inactive, rocky body orbiting the Sun − Comet - A relatively small, at times active, object whose ices can vaporize in sunlight forming an atmosphere (coma) of dust and gas and, sometimes, a tail of dust and/or gas − Meteoroid - A small particle from a comet or asteroid orbiting the Sun − Meteor - The light phenomena which results when a meteoroid enters the Earth's atmosphere and vaporizes; a shooting star − Meteorite -A meteoroid that survives its passage through the Earth's atmosphere and lands upon the Earth's surface − NEO - Near Earth Object (within 0.3 AU) − PHOs - Potentially Hazardous Objects (within 0.025 AU) COMMON DEFINITIONS 8 Copyright 2009, SpaceWorks Engineering, Inc. -
AAS/DPS Poster (PDF)
Spacewatch Observations of Asteroids and Comets with Emphasis on Discoveries by WISE AAS/DPS Poster 13.22 Thurs. 2010 Oct 7: 15:30-18:00 Robert S. McMillan1, T. H. Bressi1, J. A. Larsen2, C. K. Maleszewski1,J. L. Montani1, and J. V. Scotti1 URL: http://spacewatch.lpl.arizona.edu 1University of Arizona; 2U.S. Naval Academy Abstract • Targeted recoveries of objects discovered by WISE as well as those on impact risk pages, NEO Confirmation Page, PHAs, comets, etc. • ~1900 tracklets of NEOs from Spacewatch each year. • Recoveries of WISE discoveries preserve objects w/ long Psyn from loss. • Photometry to determine albedo @ wavelength of peak of incident solar flux. • Specialize in fainter objects to V=23. • Examination for cometary features of objects w/ comet-like orbits & objects that WISE IR imagery showed as comets. Why Targeted Followup is Needed • Discovery arcs too short to define orbits. • Objects can escape redetection by surveys: – Surveys busy covering other sky (revisits too infrequent). – Objects tend to get fainter after discovery. • Followup observations need to outnumber discoveries 10-100. • Sky density of detectable NEOs too sparse to rely on incidental redetections alone. Why Followup is Needed (cont’d) • 40% of PHAs observed on only 1 opposition. • 18% of PHAs’ arcs <30d; 7 PHAs obs. < 3d. • 20% of potential close approaches will be by objects observed on only 1 opposition. • 1/3rd of H≤22 VI’s on JPL risk page are lost and half of those were discovered within last 3 years. How “lost” can they get? • (719) Albert discovered visually in 1911. • “Big” Amor asteroid, diameter ~2 km. -
A Study of Asteroid Pole-Latitude Distribution Based on an Extended
Astronomy & Astrophysics manuscript no. aa˙2009 c ESO 2018 August 22, 2018 A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method 1 1 1 2 3 4 5 6 7 J. Hanuˇs ∗, J. Durechˇ , M. Broˇz , B. D. Warner , F. Pilcher , R. Stephens , J. Oey , L. Bernasconi , S. Casulli , R. Behrend8, D. Polishook9, T. Henych10, M. Lehk´y11, F. Yoshida12, and T. Ito12 1 Astronomical Institute, Faculty of Mathematics and Physics, Charles University in Prague, V Holeˇsoviˇck´ach 2, 18000 Prague, Czech Republic ∗e-mail: [email protected] 2 Palmer Divide Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908, USA 3 4438 Organ Mesa Loop, Las Cruces, NM 88011, USA 4 Goat Mountain Astronomical Research Station, 11355 Mount Johnson Court, Rancho Cucamonga, CA 91737, USA 5 Kingsgrove, NSW, Australia 6 Observatoire des Engarouines, 84570 Mallemort-du-Comtat, France 7 Via M. Rosa, 1, 00012 Colleverde di Guidonia, Rome, Italy 8 Geneva Observatory, CH-1290 Sauverny, Switzerland 9 Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100, Israel 10 Astronomical Institute, Academy of Sciences of the Czech Republic, Friova 1, CZ-25165 Ondejov, Czech Republic 11 Severni 765, CZ-50003 Hradec Kralove, Czech republic 12 National Astronomical Observatory, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan Received 17-02-2011 / Accepted 13-04-2011 ABSTRACT Context. In the past decade, more than one hundred asteroid models were derived using the lightcurve inversion method. Measured by the number of derived models, lightcurve inversion has become the leading method for asteroid shape determination. -
(2000) Forging Asteroid-Meteorite Relationships Through Reflectance
Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. B.S. Physics Rensselaer Polytechnic Institute, 1988 M.S. Geology and Planetary Science University of Pittsburgh, 1991 SUBMITTED TO THE DEPARTMENT OF EARTH, ATMOSPHERIC, AND PLANETARY SCIENCES IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN PLANETARY SCIENCES AT THE MASSACHUSETTS INSTITUTE OF TECHNOLOGY FEBRUARY 2000 © 2000 Massachusetts Institute of Technology. All rights reserved. Signature of Author: Department of Earth, Atmospheric, and Planetary Sciences December 30, 1999 Certified by: Richard P. Binzel Professor of Earth, Atmospheric, and Planetary Sciences Thesis Supervisor Accepted by: Ronald G. Prinn MASSACHUSES INSTMUTE Professor of Earth, Atmospheric, and Planetary Sciences Department Head JA N 0 1 2000 ARCHIVES LIBRARIES I 3 Forging Asteroid-Meteorite Relationships through Reflectance Spectroscopy by Thomas H. Burbine Jr. Submitted to the Department of Earth, Atmospheric, and Planetary Sciences on December 30, 1999 in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in Planetary Sciences ABSTRACT Near-infrared spectra (-0.90 to ~1.65 microns) were obtained for 196 main-belt and near-Earth asteroids to determine plausible meteorite parent bodies. These spectra, when coupled with previously obtained visible data, allow for a better determination of asteroid mineralogies. Over half of the observed objects have estimated diameters less than 20 k-m. Many important results were obtained concerning the compositional structure of the asteroid belt. A number of small objects near asteroid 4 Vesta were found to have near-infrared spectra similar to the eucrite and howardite meteorites, which are believed to be derived from Vesta. -
Investigating the Efficacy of Smallsats for Asteroid Detection
Investigating the Efficacy of CubeSats for Asteroid Detection Conor O’Toole 14204794 Goals • To investigate if CubeSats could be used to detect asteroids which could be classified as Near Earth Objects (NEOs), ie. that will come within 1.5AU of Earth at some point. • A number of factors must be taken into account: • Size limit on asteroids? • Max distance for detections? • One or multiple satellites? • Comparison with ground-based surveys Asteroids • Left-overs from Solar System formation • Primarily located in asteroid belts, but many occupy other orbits • Rate of collision with the planets and moons considered roughly constant • Ample evidence throughout Solar System Figure 1: Surfaces of Mercury, Moon, Mars, along with Barringer Crater in Arizona. [1], [2], [3], [4] NEOs • ~13,000 NEOs currently catalogued • 1km scale would cause destruction on a global scale. • Objects as small as 140m considered a major threat (in light of Chelyabinsk, Tunguska, etc) • Mitigation techniques in development (eg. Gravity tractor, kinetic impactor, etc) Figure 2: NEOs discovered against predicted • Primary concern remains detection values, for a range of sizes. [5] Asteroid Surveys • SpaceGuard (1998-2008) • Prioritised kilometre scale objects • CSS, LINEAR ~ 7,500 discoveries by 2014 ([6], [7]) • ATLAS (late 2015) • Early warning system for objects as small as 120m [8] • MANOS (2013-present) • Study physical parameters [9] • Space-based • NEOSSat, launched 2013 [10] • Sentinel, planned launch 2018 [11] LightForce Simulation • Space debris mitigation proposal [12-14] • Collision avoidance through ground-based laser stations • Simulation predicts roughly 90% reduction in number of collisions in the next year • Currently being extended to 100 years Figure 3: The general technique a LightForce station, either speeding up or slowing down an object to alter it’s orbit. -
Near-Earth Object Resource
NEO Resource Near-Earth Object Resource Compiled and edited by James M. Thomas for the Museum Astronomical Resource Society http://marsastro.org and the NASA/JPL Solar System Ambassador Program http://www.jpl.nasa.gov/ambassador Updated July 15, 2006 Based upon material available through the NASA Near-Earth Object Program http://neo.jpl.nasa.gov/ 1 of 104 NEO Resource Table of Contents Section Page Introduction & Overview 5 Target Earth 6 • The Cretaceous/Tertiary (K-T) Extinction 9 • Chicxulub Crater 10 • Barringer Meteorite Crater 13 What Are Near-Earth Objects (NEOs)? 14 What Is The Purpose Of The Near-Earth Object Program? 14 How Many Near-Earth Objects Have Been Discovered So Far? 15 What Is A PHA? 16 What Are Asteroids And Comets? 17 What Are The Differences Between An Asteroid, Comet, Meteoroid, Meteor and 19 Meteorite? Why Study Asteroids? 21 Why Study Comets? 24 What Are Atens, Apollos and Amors? 27 NEO Groups 28 Near-Earth Objects And Life On Earth 29 Near-Earth Objects As Future Resources 31 Near-Earth Object Discovery Teams 32 2 of 104 NEO Resource • Lincoln Near-Earth Asteroid Research (LINEAR) 35 • Near-Earth Asteroid Tracking (NEAT) 37 • Spacewatch 39 • Lowell Observatory Near-Earth Object Search (LONEOS) 41 • Catalina Sky Surveys 42 • Japanese Spaceguard Association (JSGA) 44 • Asiago DLR Asteroid Survey (ADAS) 45 Spacecraft Missions to Comets and Asteroids 46 • Overview 46 • Mission Summaries 49 • Near-Earth Asteroid Rendezvous (NEAR) 49 • DEEP IMPACT 49 • DEEP SPACE 1 50 • STARDUST 50 • Hayabusa (MUSES-C) 51 • ROSETTA -
Applying Machine Learning to Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry Kathleen Jacinda Mcintyre
University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2019 Applying Machine Learning To Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry Kathleen Jacinda Mcintyre Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Mcintyre, Kathleen Jacinda, "Applying Machine Learning To Asteroid Classification Utilizing Spectroscopically Derived Spectrophotometry" (2019). Theses and Dissertations. 2474. https://commons.und.edu/theses/2474 This Thesis is brought to you for free and open access by the Theses, Dissertations, and Senior Projects at UND Scholarly Commons. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of UND Scholarly Commons. For more information, please contact [email protected]. APPLYING MACHINE LEARNING TO ASTEROID CLASSIFICATION UTILIZING SPECTROSCOPICALLY DERIVED SPECTROPHOTOMETRY by Kathleen Jacinda McIntyre Bachelor oF Science, University oF Florida, 2011 Bachelor oF Arts, University oF Florida, 2011 A Thesis Submitted to the Graduate Faculty of the University oF North Dakota in partial fulfillment oF the reQuirements for the degree oF Master oF Science Grand Forks, North Dakota May 2019 ii PERMISSION Title ApPlying Machine Learning to Asteroid ClassiFication Utilizing SPectroscoPically Derived SPectroPhotometry DePartment Space Studies Degree Master oF Science In Presenting this thesis in Partial fulfillment of the reQuirements for a graduate degree From the University of North Dakota, I agree that the library of this University shall make it Freely available For insPection. I Further agree that permission For extensive copying For scholarly purposes may be granted by the professor Who suPervised my thesis Work, or in his absence, by the ChairPerson of the department of the dean of the School of Graduate Studies. -
Spacewatch and Follow-Up Astrometry of Near-Earth Objects
Spacewatch and Follow-up Astrometry of Near-Earth Objects International Asteroid Warning Network Steering Group Meeting Cambridge, MA 2014 Jan 13 Robert S. McMillan1, T. H. Bressi1, J. A. Larsen2, J. V. Scotti1, and R. A. Mastaler1 URL: http://spacewatch.lpl.arizona.edu 1University of Arizona; 2U.S. Naval Academy Summary • Follow-up of "large" NEOs (H≤22) as they recede from Earth after discovery and become fainter, as well as VIs, PHAs, & NEOs observed by WISE. • New, fast-reading CCD on 1.8-meter telescope. • Observed at elongations as small as 46°. • ~2800 tracklets of NEOs accepted by MPC from Spacewatch each year. • Big, long archive from 0.9-m telescope to support precoveries. Why Targeted Followup is Needed • Discovery arcs too short to define orbits: – Followup observation intervals need to be thousands of times longer than discoveries. • Objects can escape redetection by surveys: – Surveys too busy covering other sky. – Objects tend to get fainter after discovery. • Sky density of detectable NEOs is too sparse to rely on incidental redetections alone. Why More Followup is Needed • 1/3rd of PHAs observed on only 1 opposition. • 1/6th of PHAs’ arcs <30d. • ~Half of potential close approaches in the next 30 years will be by objects observed on only one opposition. • 2/3rds of H≤22 VI’s on JPL risk page are lost and > half of those were discovered within the last 6 years by modern surveys. How “lost” can they get? • (719) Albert discovered visually in 1911. • “Big” Amor asteroid, diameter ~2 km. • Favorable (perihelic) apparitions 30 yrs apart. -
Cumulative Index to Volumes 1-45
The Minor Planet Bulletin Cumulative Index 1 Table of Contents Tedesco, E. F. “Determination of the Index to Volume 1 (1974) Absolute Magnitude and Phase Index to Volume 1 (1974) ..................... 1 Coefficient of Minor Planet 887 Alinda” Index to Volume 2 (1975) ..................... 1 Chapman, C. R. “The Impossibility of 25-27. Index to Volume 3 (1976) ..................... 1 Observing Asteroid Surfaces” 17. Index to Volume 4 (1977) ..................... 2 Tedesco, E. F. “On the Brightnesses of Index to Volume 5 (1978) ..................... 2 Dunham, D. W. (Letter regarding 1 Ceres Asteroids” 3-9. Index to Volume 6 (1979) ..................... 3 occultation) 35. Index to Volume 7 (1980) ..................... 3 Wallentine, D. and Porter, A. Index to Volume 8 (1981) ..................... 3 Hodgson, R. G. “Useful Work on Minor “Opportunities for Visual Photometry of Index to Volume 9 (1982) ..................... 4 Planets” 1-4. Selected Minor Planets, April - June Index to Volume 10 (1983) ................... 4 1975” 31-33. Index to Volume 11 (1984) ................... 4 Hodgson, R. G. “Implications of Recent Index to Volume 12 (1985) ................... 4 Diameter and Mass Determinations of Welch, D., Binzel, R., and Patterson, J. Comprehensive Index to Volumes 1-12 5 Ceres” 24-28. “The Rotation Period of 18 Melpomene” Index to Volume 13 (1986) ................... 5 20-21. Hodgson, R. G. “Minor Planet Work for Index to Volume 14 (1987) ................... 5 Smaller Observatories” 30-35. Index to Volume 15 (1988) ................... 6 Index to Volume 3 (1976) Index to Volume 16 (1989) ................... 6 Hodgson, R. G. “Observations of 887 Index to Volume 17 (1990) ................... 6 Alinda” 36-37. Chapman, C. R. “Close Approach Index to Volume 18 (1991) .................. -
2014Dps...4641411M (Pdf)
SPACEWATCH® Observations of Asteroids and Comets Supporting the Large- Scale Surveys. Poster 414.11 46th Mtg of the DPS/AAS, 2014 Nov. Robert S. McMillan1, T. H. Bressi1, J. V. Scotti1, J. A. Larsen2, R. A. Mastaler1 , and A. F. Tubbiolo1 URL: http://spacewatch.lpl.arizona.edu 1University of Arizona; 2U.S. Naval Academy Photo by Marcus L. Perry, 1997 Summary • Follow-up of "large" NEOs (H≤22) as they recede from Earth after discovery and become fainter, as well as VIs, PHAs, & NEOs observed by WISE. • New, faster-reading CCD on 1.8-meter telescope. • Observed at elongations as small as 46°. • ~2800 tracklets of NEOs from Spacewatch accepted by MPC each year. • Big, long archive from 0.9-m telescope to support precoveries. Why Targeted Followup is Needed • Discovery arcs too short to define orbits: – Followup observation intervals need to be thousands of times longer than discoveries. • Objects can escape redetection by surveys: – Surveys too busy covering other sky. – Objects tend to get fainter after discovery. • Sky density of detectable NEOs is too sparse to rely on incidental redetections alone. Why More Followup is Needed • 1/3rd of PHAs observed on only 1 opposition. • 1/6th of PHAs’ arcs <30d. • ~Half of potential close approaches in the next 30 years will be by objects observed on only one opposition. • 2/3rds of H≤22 VI’s on JPL risk page are lost and > half of those were discovered within the last 6 years by modern surveys. How “lost” can they get? • (719) Albert discovered visually in 1911. • “Big” Amor asteroid, diameter ~2 km. -
Life in a Shooting Gallery Meteors, Meteorites, and Meteoroids
Life in a Shooting Gallery Meteors, Meteorites, and Meteoroids • Meteor: the streak of light seen in the sky • Meteorite: the rock found on the ground • Meteoroid: the rock before it hits Earth Meteorites are easily-studied remnants of the formation of the solar system Meteors “It is easier to believe that Yankee professors would lie than that stones would fall from heaven.” -- attributed to Thomas Jefferson From below … Meteors … and above Meteors • Most are the size of a grain of sand • They vaporize about 75-100 km up when they hit the atmosphere • Impact velocities >20 km/s • The trails are ionized gas • Best viewed after midnight Meteor Showers Occur when Earth passes through the orbit of a comet. Examples: • Orionids: comet 1P/Halley Oct 21-22 • Leonids: comet 109P/Tempel-Tuttle Nov 17-18 • Geminids: asteroid 3200 Phaeton Dec 13-14 • Perseids: comet 55P/Swift-Tuttle Aug 12-13 • Lyrids: comet Thatcher Apr 22-23 Orbits of Meteor Showers Fireballs and Bolides • Very bright meteors • May leave a persistent trail • Due to impacting object bigger than about 1m Geminid Fireball 12/9/2010. source: S. Korotkiy, Russian Academy of Sciences Grand Tetons Meteor 8/10/72. 3-14m Apollo asteroid. V=15 km/s; 15km altitude Bering Sea Bolide Dec 18, 2018. 170 kT explosion. 26 km height Source: NASA Peekskill Meteorite 10/9/92 12 kg Stony-Iron Classification S C M Primitive meteorites (chondrites) Unchanged since solar system formation • Stony: rocky minerals + small fraction of metal flakes • Carbonaceous (Carbon-rich): like stony, with large amounts -
The Vector Alignments of Asteroid Spins by Thermal Torques
articles The vector alignments of asteroid spins by thermal torques David Vokrouhlicky´1, David Nesvorny´2 & William F. Bottke2 1Institute of Astronomy, Charles University, V Holesˇovicˇka´ch 2, 180 00 Prague 8, Czech Republic 2Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, Colorado 80302, USA ........................................................................................................................................................................................................................... Collisions have been thought to be the dominant process altering asteroid rotations, but recent observations of the Koronis family of asteroids suggest that this may be incorrect. This group of asteroids was formed in a catastrophic collision several billion years ago; in the intervening period their rotational axes should have become nearly random because of subsequent collisions, with spin rates that follow a maxwellian distribution. What is seen, however, is that the observed family members with prograde spins have nearly identical periods (7.5–9.5 h) and obliquities between 42 and 50 degrees, while those with retrograde spins have obliquities between 154 and 169 degrees with periods either <5hor>13 h. Here we show that these non-random orientations and spin rates can be explained by ‘thermal torques’ (arising from differential solar heating), which modify the spin states over time. In some cases, the asteroids become trapped in spin-orbit resonances. Our results suggest that thermal torques may be more important than collisions in changing the spin states (and possibly shapes) of asteroids with diameters <40 km. Asteroid families are by-products of catastrophic disruption events Slivan’s solutions have been verified in two different ways. First of (for example, ref. 1). They are identified by the clustered proper all, his analysis yielded a spin vector for (243) Ida that agrees with semimajor axis a, eccentricity e, and inclination I values of their spacecraft observations17,18.