Statistical Survey and Analysis of Photometric and Spectroscopic Data on Neas
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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. -
Photometric Study of Two Near-Earth Asteroids in the Sloan Digital Sky Survey Moving Objects Catalog
University of North Dakota UND Scholarly Commons Theses and Dissertations Theses, Dissertations, and Senior Projects January 2020 Photometric Study Of Two Near-Earth Asteroids In The Sloan Digital Sky Survey Moving Objects Catalog Christopher James Miko Follow this and additional works at: https://commons.und.edu/theses Recommended Citation Miko, Christopher James, "Photometric Study Of Two Near-Earth Asteroids In The Sloan Digital Sky Survey Moving Objects Catalog" (2020). Theses and Dissertations. 3287. https://commons.und.edu/theses/3287 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]. PHOTOMETRIC STUDY OF TWO NEAR-EARTH ASTEROIDS IN THE SLOAN DIGITAL SKY SURVEY MOVING OBJECTS CATALOG by Christopher James Miko Bachelor of Science, Valparaiso University, 2013 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 August 2020 Copyright 2020 Christopher J. Miko ii Christopher J. Miko Name: Degree: Master of Science This document, submitted in partial fulfillment of the requirements for the degree from the University of North Dakota, has been read by the Faculty Advisory Committee under whom the work has been done and is hereby approved. ____________________________________ Dr. Ronald Fevig ____________________________________ Dr. Michael Gaffey ____________________________________ Dr. Wayne Barkhouse ____________________________________ Dr. Vishnu Reddy ____________________________________ ____________________________________ This document is being submitted by the appointed advisory committee as having met all the requirements of the School of Graduate Studies at the University of North Dakota and is hereby approved. -
Asteroids + Comets
Datasets for Asteroids and Comets Caleb Keaveney, OpenSpace intern Rachel Smith, Head, Astronomy & Astrophysics Research Lab North Carolina Museum of Natural Sciences 2020 Contents Part 1: Visualization Settings ………………………………………………………… 3 Part 2: Near-Earth Asteroids ………………………………………………………… 5 Amor Asteroids Apollo Asteroids Aten Asteroids Atira Asteroids Potentially Hazardous Asteroids (PHAs) Mars-crossing Asteroids Part 3: Main-Belt Asteroids …………………………………………………………… 12 Inner Main Asteroid Belt Main Asteroid Belt Outer Main Asteroid Belt Part 4: Centaurs, Trojans, and Trans-Neptunian Objects ………………………….. 15 Centaur Objects Jupiter Trojan Asteroids Trans-Neptunian Objects Part 5: Comets ………………………………………………………………………….. 19 Chiron-type Comets Encke-type Comets Halley-type Comets Jupiter-family Comets C 2019 Y4 ATLAS About this guide This document outlines the datasets available within the OpenSpace astrovisualization software (version 0.15.2). These datasets were compiled from the Jet Propulsion Laboratory’s (JPL) Small-Body Database (SBDB) and NASA’s Planetary Data Service (PDS). These datasets provide insights into the characteristics, classifications, and abundance of small-bodies in the solar system, as well as their relationships to more prominent bodies. OpenSpace: Datasets for Asteroids and Comets 2 Part 1: Visualization Settings To load the Asteroids scene in OpenSpace, load the OpenSpace Launcher and select “asteroids” from the drop-down menu for “Scene.” Then launch OpenSpace normally. The Asteroids package is a big dataset, so it can take a few hours to load the first time even on very powerful machines and good internet connections. After a couple of times opening the program with this scene, it should take less time. If you are having trouble loading the scene, check the OpenSpace Wiki or the OpenSpace Support Slack for information and assistance. -
198 5MNRAS.212. .817S Mon. Not. R. Astr. Soc. (1985
Mon. Not. R. astr. Soc. (1985) 212, 817-836 .817S 5MNRAS.212. Collisions in the Solar System -1. 198 Impacts of the Apollo-Amor-Aten asteroids upon the terrestrial planets Duncan I. Steel and W. J. Baggaley Department of Physics, University of Canterbury, Christchurch, New Zealand Accepted 1984 September 26. Received 1984 September 14; in original form 1984 July 11 Summary. The collision probability between each of the presently-known population of four Aten, 34 Apollo and 38 Amor asteroids and each of the terrestrial planets is determined by a new technique. The resulting mean collision rates, coupled with estimates of the total undiscovered population of each class, is useful in calculating the rate of removal of these bodies by the terrestrial planets, and the cratering rate on each planet by bodies of diameter in excess of 1 km. The influx to the Earth is found to be one impact per 160 000 yr, but this figure is biased by the inclusion of four recently-discovered low-inclination Apollos. Excluding these four the rate would be one per 250 000 yr, in line with previous estimates. The impact rate is highest for the Earth, being around twice that of Venus. The rates for Mercury and Mars using the present sample are about one per 5 Myr and one per 1.5 Myr respectively. 1 Introduction Over the past two decades our knowledge of the asteroids has expanded greatly. Physical studies of these bodies, reviewed by Chapman, Williams & Hartman (1978), Chapman (1983) and in Gehrels (1979), have shown that distinct groups of common genesis exist. -
Planet Formation
ƴÚˎ͛́ɓ (planet formation) ́D͟ ȓȓȓȓ 1111 þþþþ ĭĭĭĭ ɋɋɋɋ IIII ĤĤĤĤ ͓͓͓͓ &&&& ̤̤̤̤ The Solar System Planets are almost on the same plane. Planets orbit the Sun in the same direction. The Sun is rotating in the same direction as the planets’ orbital movement. Planets form in a disk! 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 2 SScceennaarriioo ooff SSttaarr && PPllaanneett ffoorrmmaattiioonn ƉƉƉƉ ͭͭͭͭ ǥǥǥǥ DDDD ³³³³ ǟǟǟǟ ΩΩΩΩ ³³³³ šššš ³³³³ ɋɋɋɋ ÕÕÕÕ Molecular Cloud 3̮ NJNJNJNJ ˠˠˠˠ ³³³³ ƦÀ͌ ʴʴʴʴ ÜÜÜÜ A star is made of gas star formation needs gas a star forming region is full of dense gas and dust (NJNJ ɁɁ ). Formation of the Solar System 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 4 Formation of planetesimals 20 micron 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 5 Formation of planets closer to the Sun, warm, no ice Far from the Sun, cold, Ice helps to grow a big solid core gas accretion 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 6 -³ j É ϕ ƴ Ú ƽ > ³ ɷ > ³ The Solar System ȳ ȳ ȳ ȳ ˚ ˚ ˚ ˚ ǯ ǯ ǯ ǯ Ω Ω Ω Ω Ź Ź Ź Ź ˙ǚ@ƍ: Ð Ð Ð Ð http://www.gps.caltech.edu/ ~mbrown/ ͧI2Ω006̛ /11ʍ /1 ̮ ¹Ǥėɓ ɓ nj ƭ ƴ Ú 7 PPlluuttoo:: tthhee 99tthh ppllaanneett?? by Hubble Space telescope 1 AU (astronomical unit) Distance to Sun =earth-to-Sun distance 39.5 AU Eris (satellite: Dysnomia) 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 8 Orbit of Eris side view top view http://bobthealien.co.uk/eris.htm 2006/11/1 ¹Ǥėɓ ɓ nj ƭ ƴ Ú 9 NNeeww PPllaanneett DDeeffiinniittiioonn http://www.iau2006.org/mirror/www.iau.org/iau0603/index.html © orbit a star (upper mass limit: brown dwarf Υǖɓ, no nuclear fusion?) © massive enough to keep a round shape (lower mass limit: about 5x1023 g or ȂȂȂȂ ιιιι >400 km ?) © has cleared the neighborhood around its orbit. -
(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. -
1987Aj 93. . 738T the Astronomical Journal
738T . THE ASTRONOMICAL JOURNAL VOLUME 93, NUMBER 3 MARCH 1987 93. DISCOVERY OF M CLASS OBJECTS AMONG THE NEAR-EARTH ASTEROID POPULATION Edward F. TEDEScoa),b) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, California 91109 1987AJ Jonathan Gradie20 Planetary Geosciences Division, Hawaii Institute of Geophysics, University of Hawaii, Honolulu, Hawaii 96822 Received 10 September 1986; revised 17 November 1986 ABSTRACT Broadband colorimetry (0.36 to 0.85 ¡um), visual photometry, near-infrared (JHK) photometry, and 10 and 20 /urn radiometry of the near-Earth asteroids 1986 DA and 1986 EB were obtained during March and April 1986. Model radiometric visual geometric albedos of 0.14 + 0.02 and 0.19 + 0.02 and model radiometric diameters of 2.3 + 0.1 and 2.0 + 0.1 km, respectively, (on the IRAS asteroid ther- mal model system described by Lebofsky et al. 1986) were derived from the thermal infrared and visual fluxes. These albedos, together with the colorimetric and (for 1986 DA) near-infrared data, establish that both objects belong to the M taxonomic class, the first of this kind to be recognized among the near-Earth asteroid population. This discovery, together with previous detections of C and S class objects, establishes that all three of the most common main-belt asteroid classes are represented among this population. The similarity in the corrected distribution of taxonomic classes among the 38 Earth- approaching asteroids for which such classes exist is similar to those regions of the main belt between the 3:1 (2.50 AU) and 5:2 (2.82 AU) orbital resonances with Jupiter, suggesting that they have their origins among asteroids in the vicinity of these resonances. -
Aten-Alinda Orbital Evolution: the Example of Possible Interacting Orbits
ATEN-ALINDA ORBITAL EVOLUTION: THE EXAMPLE OF POSSIBLE INTERACTING ORBITS A. Rosaev FGUP NPC "NEDRA" Minor planets 887 Alinda and 2062 Aten are typical 1. INTRODUCTION near Earth asteroids (NEA). Our previous researches show their possible origin in catastrophic collision near Minor planets 887 Alinda and 2062 Aten are typical Earth orbit. It is determine the target of present near earth objects ((NEA). They represent different research – to investigate interactions between these dynamical groups of NEA, Amor's and Aten's groups objects in more details. accordingly. The origin of Aten's group has a particular Orbits m.p. 887 and 2062 are crossed near pericenter interest due to specific character of their orbits. The and apocenter accordingly. So possible interval of the elements of orbits m.p. 887 and 2062 are given in the interaction of these objects is repeated through the table 1. significant time interval and has relatively small Orbits m.p. 887 and 2062 are crossed near pericenter duration. and apocenter accordingly (Fig.1). So possible interval On the strength of several reasons, orbits of fragments of the interaction of these objects is repeated through of the disastrous collision can have no an exact the significant time interval and has relatively small intersection. Besides, when integrating on the greater duration. gap in the past increases a role of the uncertainty of Table1 initial values of elements of orbits. These factors Aten – Alinda orbital elements determine a probabilistic nature of the result as well as need of modeling of the disastrous process. However, on the strength of the specific spatial location of orbits, Element Aten Alinda result has highly determined numeric expression - in q 0.79 1.08 the suggestion on the possible interaction m. -
– Near-Earth Asteroid Mission Concept Study –
ASTEX – Near-Earth Asteroid Mission Concept Study – A. Nathues1, H. Boehnhardt1 , A. W. Harris2, W. Goetz1, C. Jentsch3, Z. Kachri4, S. Schaeff5, N. Schmitz2, F. Weischede6, and A. Wiegand5 1 MPI for Solar System Research, 37191 Katlenburg-Lindau, Germany 2 DLR, Institute for Planetary Research, 12489 Berlin, Germany 3 Astrium GmbH, 88039 Friedrichshafen, Germany 4 LSE Space AG, 82234 Oberpfaffenhofen, Germany 5 Astos Solutions, 78089 Unterkirnach, Germany 6 DLR GSOC, 82234 Weßling, Germany ASTEX Marco Polo Symposium, Paris 18.5.09, A. Nathues - 1 Primary Objectives of the ASTEX Study Identification of the required technologies for an in-situ mission to two near-Earth asteroids. ¾ Selection of realistic mission scenarios ¾ Definition of the strawman payload ¾ Analysis of the requirements and options for the spacecraft bus, the propulsion system, the lander system, and the launcher ASTEX ¾ Definition of the requirements for the mission’s operational ground segment Marco Polo Symposium, Paris 18.5.09, A. Nathues - 2 ASTEX Primary Mission Goals • The mission scenario foresees to visit two NEAs which have different mineralogical compositions: one “primitive'‘ object and one fragment of a differentiated asteroid. • The higher level goal is the provision of information and constraints on the formation and evolution history of our planetary system. • The immediate mission goals are the determination of: – Inner structure of the targets – Physical parameters (size, shape, mass, density, rotation period and spin vector orientation) – Geology, mineralogy, and chemistry ASTEX – Physical surface properties (thermal conductivity, roughness, strength) – Origin and collisional history of asteroids – Link between NEAs and meteorites Marco Polo Symposium, Paris 18.5.09, A. -
Minerals in Meteorites
APPENDIX 1 Minerals in Meteorites Minerals make up the hard parts of our world and the Solar System. They are the building blocks of all rocks and all meteorites. Approximately 4,000 minerals have been identified so far, and of these, ~280 are found in meteorites. In 1802 only three minerals had been identified in meteorites. But beginning in the 1960s when only 40–50 minerals were known in meteorites, the discovery rate greatly increased due to impressive new analytic tools and techniques. In addition, an increasing number of different meteorites with new minerals were being discovered. What is a mineral? The International Mineralogical Association defines a mineral as a chemical element or chemical compound that is normally crystalline and that has been formed as a result of geological process. Earth has an enormously wide range of geologic processes that have allowed nearly all the naturally occurring chemical elements to participate in making minerals. A limited range of processes and some very unearthly processes formed the minerals of meteorites in the earliest history of our solar system. The abundance of chemical elements in the early solar system follows a general pattern: the lighter elements are most abundant, and the heavier elements are least abundant. The miner- als made from these elements follow roughly the same pattern; the most abundant minerals are composed of the lighter elements. Table A.1 shows the 18 most abundant elements in the solar system. It seems amazing that the abundant minerals of meteorites are composed of only eight or so of these elements: oxygen (O), silicon (Si), magnesium (Mg), iron (Fe), aluminum (Al), calcium (Ca), sodium (Na) and potas- sium (K). -
9781107061446 Index.Pdf
Cambridge University Press 978-1-107-06144-6 - Asteroids: Relics of Ancient Time Michael K. Shepard Index More information Index absolute magnitude binary, see asteroids, moons correlation with asteroid size 289 Centaurs, see Centaurs definition 45 classification, see asteroid classification search program limits 288, 295 Edgeworth–Kuiper belt, see trans- stellar 45 Neptunian objects achondrite families, see Hirayama families aubrite, see enstatite achondrite Hildas 65 definition 113 naming conventions 28 diogenite 114 near-Earth, see near-Earth asteroids eucrite 113 origin of term 13 exotic or unusual 115 regolith 122 howardite 114 satellites, see asteroids, moons howardite–eucrite–diogenite 114, 127, search programs, see asteroid search 274 programs irons, see iron meteorites spectra, see specific asteroids lunar 120 threats, see impacts Martian 119 trans-Neptunian object, see trans- mesosiderite 116 Neptunian object pallasite, see pallasites Trojan 19–20 primitive 115 asteroids, moons shergotite–nakhlite–chassignite 119 45 Eugenia 244 urelite 5, 115 87 Sylvia 245 adaptive optics 90 Antiope 244 definition 44 243 Ida and Dactyl 243 guide star 225 762 Pulcova 245 operation 224–5 185851 2000 DP107 245 resolution 225 2001 SN263 245 albedo, visual 48 discovery methods 245 Alvarez, Walter and Luis 132 formation mechanisms 246–7 Apophis, asteroid 99942 population reservoirs 245 discovery 283 asteroids, number and name history of threat 283–4 1 Ceres, see Ceres, asteroid 1 size 283 2 Pallas, see Pallas, asteroid 2 Torino scale 293 3 Juno 15 Arnold, Steve 97 4 Vesta, see Vesta, asteroid 4 asteroids 21 Lutetia, see Lutetia, asteroid 21 albedo 48 45 Eugenia 244 Amor, see near-Earth asteroids 87 Sylvia 245 Aten, see near-Earth asteroids 90 Antiope 244 Apollo, see near-Earth asteroids 135 Hertha 230 Atira, Aphohele, see near-Earth asteroids 243 Ida and Dactyl 243 341 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-06144-6 - Asteroids: Relics of Ancient Time Michael K. -
Detection of Semimajor Axis Drifts in 54 Near-Earth Asteroids: New Measurements of the Yarkovsky Effect
The Astronomical Journal, 144:60 (13pp), 2012 August doi:10.1088/0004-6256/144/2/60 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DETECTION OF SEMIMAJOR AXIS DRIFTS IN 54 NEAR-EARTH ASTEROIDS: NEW MEASUREMENTS OF THE YARKOVSKY EFFECT C. R. Nugent1, J. L. Margot1,2,S.R.Chesley3, and D. Vokrouhlicky´ 4 1 Department of Earth and Space Sciences, University of California, Los Angeles, CA 90095, USA 2 Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA 3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA 4 Institute of Astronomy, Charles University, V Holesovi˘ ck˘ ach´ 2, CZ-18000 Prague 8, Czech Republic Received 2012 April 16; accepted 2012 June 7; published 2012 July 12 ABSTRACT We have identified and quantified semimajor axis drifts in near-Earth asteroids (NEAs) by performing orbital fits to optical and radar astrometry of all numbered NEAs. We focus on a subset of 54 NEAs that exhibit some of the most reliable and strongest drift rates. Our selection criteria include a Yarkovsky sensitivity metric that quantifies the detectability of semimajor axis drift in any given data set, a signal-to-noise metric, and orbital coverage requirements. In 42 cases, the observed drifts (∼10−3 AU Myr−1) agree well with numerical estimates of Yarkovsky drifts. This agreement suggests that the Yarkovsky effect is the dominant non-gravitational process affecting these orbits, and allows us to derive constraints on asteroid physical properties. In 12 cases, the drifts exceed nominal Yarkovsky predictions, which could be due to inaccuracies in our knowledge of physical properties, faulty astrometry, or modeling errors.