DOCSLIB.ORG

Spectral Properties of Near-Earth Asteroids: Evidence for Sources of Ordinary Chondrite Meteorites Author(S): Richard P

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Spectral Properties of Near-Earth Asteroids: Evidence for Sources of Ordinary Chondrite Meteorites Author(s): Richard P. Binzel, Schelte J. Bus, Thomas H. Burbine and Jessica M. Sunshine Reviewed work(s): Source: Science, New Series, Vol. 273, No. 5277 (Aug. 16, 1996), pp. 946-948 Published by: American Association for the Advancement of Science Stable URL: http://www.jstor.org/stable/2891527 . Accessed: 18/12/2012 11:25 Your use of the JSTOR archive indicates your acceptance of the Terms & Conditions of Use, available at . http://www.jstor.org/page/info/about/policies/terms.jsp . JSTOR is a not-for-profit service that helps scholars, researchers, and students discover, use, and build upon a wide range of content in a trusted digital archive. We use information technology and tools to increase productivity and facilitate new forms of scholarship. For more information about JSTOR, please contact [email protected]. American Association for the Advancement of Science is collaborating with JSTOR to digitize, preserve and extend access to Science. http://www.jstor.org This content downloaded on Tue, 18 Dec 2012 11:25:44 AM All use subject to JSTOR Terms and Conditions close to the A+ direction obtained from tipodalpositive inclination in the marginof 3. A. Kroner and P. W. Layer, Science 256, 1405 of the to- the in the (1992). the margin Kaap Valley pluton pluton and sedimentsadjacent to 4. E. S. Barton, W. Altermann, I. S. Williams, C. B. nalite and reflects overprinting of the pluton(which is presentto a lesserdegree in Smith, Geology 22, 343 (1994). Moodiesshale duringpluton emplacement. the pluton interior).This directionis signif- 5. L. J. Robb, J. M. Barton Jr., E. J. D. Kable, R. C. Zirconfrom a dikefrom the CluthaMine icantly differentfrom the present-daymag- Wallace, Precambrian Res. 31, 1 (1986). 6. A. R. Tegtmeyer and A. Kr6ner,ibid. 36, 1 (1987); R. (Fig. 1) that crosscutsthe folded Moodies netic field directionand cannot be correlat- A. Armstrong, W. Compston, M. J. de Wit, I. S. sedimentshas a single-grainPb-Pb age of ed with the timing of later thermalevents Williams,Earth Planet. Sci. Lett. 101, 90 (1990); S. L. 3224.5 ? 0.4 Ma (Table3), indicatingthat that could have caused a magnetic over- Kamo, D. W. Davis,:M. J. de Wit, Geol. Soc. Aust. the Moodies was folded before this time. printing.We believe this is a primarymag- Abstr. Ser. 23, 53 (1990). 7. J. L. Kirschvink,Geophys. J. R. Astron. Soc. 62, 699 Becausethe A magnetizationwas acquired netization, acquiredduring cooling of the (1980). afterfolding, it is thereforeonly constrained pluton at 3214 Ma. The data suggestthat a 8. D. R. Van Alstine, ibid. 61, 101 (1979). to be youngerthan 3224 Ma and maycoin- reversal of Earth's magnetic field is pre- 9. P. J. Hattingh, thesis, Universityof Pretoria (1983). cide with the hornblendeage of 3214 Ma. servedin the KaapValley pluton, making it 10. R. B. Hargraves, J. Geol. 78, 253 (1970); 11. P. W. Layer, A. Krbner,M. McWilliams,N. Clauer, J. Our paleomagneticstudy of the Kaap the oldest observedreversal and implying Geophys. Res. 93, 2191 (1988). Valley pluton shows two distinct magnetic that the reversinggeomagnetic dynamo has 12. P. W. Layer, -M. 0. McWilliams,A. Krbner,Eos 45, directions.One is positive inclinationthat been operatingsince the earlyArchean. 689 (1983); P. W. Layer, A. Kr6ner, D. York, M. 0. correspondsto an overprintdirection caused McWilliams,ibid. 70, 1064 (1989). 13. P. W. Layer, A. Kroner, M. McWilliamsA. Burghele, by the intrusionof presumedearly Protero- REFERENCES J. Geophys. Res. 93, 449 (1988). zoic dikes and is seen in both the interior 14. R. A. Fisher, Proc. R. Soc. London Ser. A 217, 295 and marginof the pluton. The other direc- 1. M. W. McElhinnyand W. E. Senanayake, J. Geo- (1953). tion is characterizedby a negative inclina- phys. Res. 85, 3523 (1980); C. J. Hale and D. J. 15. A. Kr6ner, G. R. Byerly, D. R. Lowe, Earth Planet. Dunlop, Geophys. Res. Lett. 11, 97 (1984). Sci. Lett. 103, 41 (1991). tion in the interiorof the pluton (which is 2. P. W. Layer, A. Kroner, D. York, Geology 20, 717 absentfrom the pluton margin)and an an- (1992). 25 March 1996; accepted 13 June 1996 lation of small objects distinct from the Spectral Properties of Near-EarthAsteroids: S-class asteroids(8). Our observationsdo Evidence for Sources of Ordinary not reveal a distinct populationof Q-class objects amongsmall near-Earthasteroids. Chondrite Meteorites We madespectroscopic measurements of RichardP. Binzel, Schelte J. Bus, Thomas H. Burbine, 35 near-Earthasteroids, which we have ob- tainedas target-of-opportunityobservations Jessica M. Sunshine over 1991 through 1996. In making these observations,we useda low-resolutionspec- Although ordinary chondrite (OC) meteorites dominate observed falls, the identification of trographand solid-statecharge-coupled de- near-Earth and main-belt asteroid sources has remained elusive. Telescopic measure- vice (CCD) detectorsattached to the 2.4-m ments of 35 near-Earth asteroids (-3 kilometers in diameter) revealed six that have visible Hiltner telescope of the Michigan-Dart- wavelength spectra similar to laboratory spectra of OC meteorites. Near-Earth asteroids mouth-MassachusettsInstitute of Technol- were found to have spectral properties that span the range between the previously sep- ogy (MDM) Observatoryat Kitt Peak, Ar- arated domains of OC meteorites and the most common (S class) asteroids, suggesting izona (9). Our spectra cover the visible- a link.This range of spectral properties could arise through a diversity of mineralogies and wavelength range from 0.45 to 0.95 pm. regolith particle sizes, as well as through a time-dependent surface weathering process. Over these wavelengths,most of the aster- oids categorizedwithin the S classand most of the near-Earthasteroids we measured displayspectra with a moderateabsorption Of the meteoritesfalling to Earth,80% are magnitudes,and limitedintervals of visibility. band near 1 pLm,which arisesowing to the stones consistingof olivine and pyroxene, Of these measuredasteroids, only one (1862 presenceof olivine and pyroxene(10, 11). which are classifiedas ordinarychondrites Apollo) has spectralproperties widely recog- However,six of the near-Earthasteroids we (OCs).They are thought to representsamples nized as similar to the laboratoryspectral measuredhave spectrathat displayunusu- of the primitivesolar nebula that have under- propertiesof OC meteorites(4-6). We now ally deep I-rim absorptionbands (Fig. 1). gone modestthermal evolution over the age reportthe resultsof a surveyof the visible- Over our measuredwavelength range, the of the solarsystem (1). The most immediate wavelengthspectral properties of near-Earth spectraof these near-Earthasteroids do not sourcesfor meteoritesare likely to be near- asteroids:we find manythat appearto have resemble4 Vesta (Fig. IA), but they do Earthasteroids (2), which in turnare derived spectrasimilar to OC meteorites. appearsimilar to the spectraof 349 Dem- predominantlyfrom the main asteroidbelt There has also been a long-standingde- bowskaand 1862 Apollo (Fig. I B) (l 2, 13). (3). Relativelyfew spectroscopicobservations bate over whetherthe most commonlyob- Although Dembowskaand Apollo clearly of near-Earthasteroids have been obtained served (S class) asteroidsare relatedto the have distinguishablehear-infrared spectra becauseof their small sizes, faint apparent most commonmeteorites, in spite of a mis- (14), such measurementsfor our set of faint match in their red spectralslopes and ab- near-Earthasteroids are not yet available. R. P. Binzel, S. J. Bus, T. H. Burbine, Department of Earth, sorption band depths. One hypothesisfor We makean inferencefor the spectraof our Atmospheric, and PlanetarySciences, Massachusetts In- stitute of Technology, Cambridge, MA 02139, USA. this spectralmismatch is that some "space set of near-Earthasteroids by considering J. M. Sunshine, Department of Earth, Atmospheric, and weathering"process is responsiblefor alter- the mineralogies(based on near-infrared Planetary Sciences, Massachusetts Instituteof Technol- ing the spectralproperties of OC asteroids measurements)and meteorite analogs for ogy, Cambridge, MA 02139, and Science Applications InternationalCorporation, 4501 Daly Drive, Chantilly,VA (7). Another hypothesisis that Apollo-like Dembowska and Apollo. Dembowska is 22021, USA. OC asteroids(the Q class) exist as a popu- consideredto be a pyroxene-olivineassem- 946 SCIENCE * VOL.273 * 16 AUGUST 1996 This content downloaded on Tue, 18 Dec 2012 11:25:44 AM All use subject to JSTOR Terms and Conditions &WREPORTS blagewith little or no metal (14). Apollo is given our spectralcoverage, we are not able oids have estimated diametersof -3 km; interpretedto have a metal, olivine, and to distinguishamong H, L, or LL chondrite these objectsare thus the smallestasteroids pyroxenemineralogy similar to that of OC analogsfor these near-Earthasteroids. that have been spectrallymeasured to date meteorites(5). Given that Dembowskais In addition to identifyingsix potential (17). One possibilityfor the continuumof an outer main-beltasteroid.with no known OC-like near-Earthasteroids (Fig. 2), we spectralproperties is that asteroidsin this dynamicallink to the inner solar system found 29 that have spectralproperties in- size range are more likely than are larger and that no Dembowska-likemeteorites are termediatebetween those of S asteroidsand asteroidsto be composedof distinct litho- present in our collections (15), we infer those of OC meteorites(Fig. 3, A and B). logic
Recommended publications
  • Planet Positions: 1 Planet Positions

    Planet Positions: 1 Planet Positions

    Planet Positions: 1 Planet Positions As the planets orbit the Sun, they move around the celestial sphere, staying close to the plane of the ecliptic. As seen from the Earth, the angle between the Sun and a planet -- called the elongation -- constantly changes. We can identify a few special configurations of the planets -- those positions where the elongation is particularly noteworthy. The inferior planets -- those which orbit closer INFERIOR PLANETS to the Sun than Earth does -- have configurations as shown: SC At both superior conjunction (SC) and inferior conjunction (IC), the planet is in line with the Earth and Sun and has an elongation of 0°. At greatest elongation, the planet reaches its IC maximum separation from the Sun, a value GEE GWE dependent on the size of the planet's orbit. At greatest eastern elongation (GEE), the planet lies east of the Sun and trails it across the sky, while at greatest western elongation (GWE), the planet lies west of the Sun, leading it across the sky. Best viewing for inferior planets is generally at greatest elongation, when the planet is as far from SUPERIOR PLANETS the Sun as it can get and thus in the darkest sky possible. C The superior planets -- those orbiting outside of Earth's orbit -- have configurations as shown: A planet at conjunction (C) is lined up with the Sun and has an elongation of 0°, while a planet at opposition (O) lies in the opposite direction from the Sun, at an elongation of 180°. EQ WQ Planets at quadrature have elongations of 90°.
  • Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur

    Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur

    Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes.
  • Temperature-Induced Effects and Phase Reddening on Near-Earth Asteroids

    Temperature-Induced Effects and Phase Reddening on Near-Earth Asteroids

    Planetologie Temperature-induced effects and phase reddening on near-Earth asteroids Inaugural-Dissertation zur Erlangung des Doktorgrades der Naturwissenschaften im Fachbereich Geowissenschaften der Mathematisch-Naturwissenschaftlichen Fakultät der Westfälischen Wilhelms-Universität Münster vorgelegt von Juan A. Sánchez aus Caracas, Venezuela -2013- Dekan: Prof. Dr. Hans Kerp Erster Gutachter: Prof. Dr. Harald Hiesinger Zweiter Gutachter: Dr. Vishnu Reddy Tag der mündlichen Prüfung: 4. Juli 2013 Tag der Promotion: 4. Juli 2013 Contents Summary 5 Preface 7 1 Introduction 11 1.1 Asteroids: origin and evolution . 11 1.2 The asteroid-meteorite connection . 13 1.3 Spectroscopy as a remote sensing technique . 16 1.4 Laboratory spectral calibration . 24 1.5 Taxonomic classification of asteroids . 31 1.6 The NEA population . 36 1.7 Asteroid space weathering . 37 1.8 Motivation and goals of the thesis . 41 2 VNIR spectra of NEAs 43 2.1 The data set . 43 2.2 Data reduction . 45 3 Temperature-induced effects on NEAs 55 3.1 Introduction . 55 3.2 Temperature-induced spectral effects on NEAs . 59 3.2.1 Spectral band analysis of NEAs . 59 3.2.2 NEAs surface temperature . 59 3.2.3 Temperature correction to band parameters . 62 3.3 Results and discussion . 70 4 Phase reddening on NEAs 73 4.1 Introduction . 73 4.2 Phase reddening from ground-based observations of NEAs . 76 4.2.1 Phase reddening effect on the band parameters . 76 4.3 Phase reddening from laboratory measurements of ordinary chondrites . 82 4.3.1 Data and spectral band analysis . 82 4.3.2 Phase reddening effect on the band parameters .
  • Physical Properties of Near-Earth Asteroids

    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.
  • 1. Some of the Definitions of the Different Types of Objects in the Solar

    1. Some of the Definitions of the Different Types of Objects in the Solar

    1. Some of the definitions of the different types of objects in has the greatest orbital inclination (orbit at the the solar system overlap. Which one of the greatest angle to that of Earth)? following pairs does not overlap? That is, if an A) Mercury object can be described by one of the labels, it B) Mars cannot be described by the other. C) Jupiter A) dwarf planet and asteroid D) Pluto B) dwarf planet and Kuiper belt object C) satellite and Kuiper belt object D) meteoroid and planet 10. Of the following objects in the solar system, which one has the greatest orbital eccentricity and therefore the most elliptical orbit? 2. Which one of the following is a small solar system body? A) Mercury A) Rhea, a moon of Saturn B) Mars B) Pluto C) Earth C) Ceres (an asteroid) D) Pluto D) Mathilde (an asteroid) 11. What is the largest moon of the dwarf planet Pluto 3. Which of the following objects was discovered in the called? twentieth century? A) Chiron A) Pluto B) Callisto B) Uranus C) Charon C) Neptune D) Triton D) Ceres 12. If you were standing on Pluto, how often would you see 4. Pluto was discovered in the satellite Charon rise above the horizon each A) 1930. day? B) 1846. A) once each 6-hour day as Pluto rotates on its axis C) 1609. B) twice each 6-hour day because Charon is in a retrograde D) 1781. orbit C) once every 2 days because Charon orbits in the same direction Pluto rotates but more slowly 5.
  • Jjmonl 1710.Pmd

    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 ...............................................................
  • Dealing with the Threat of an Asteroid Striking the Earth

    Dealing with the Threat of an Asteroid Striking the Earth

    Dealing with the Threat of an Asteroid Striking the Earth An AIAA Position Paper April 1990 This paper originated in the AIAA Space Systems Technical Committee and was Approved by the AIAA Board of Directors American Institute of Aeronautics and Astronautics 1801 Alexander Bell Drive Reston, VA 20191 703/264-7500 SUMMARY Hundreds, perhaps thousands, of asteroids travel in orbits that intersect the Earth’s orbit. Some have struck the Earth in the past, leaving large craters. Others have come very close, one as recently as March 23, 1989 (Apollo Asteroid 1989FC, estimated to be a fifth to a half mile in diameter). Such an object, if it struck the Earth today, could cause a disaster of unprecedented proportions. Although the probability of such an occurrence is very small, its consequences (i.e., the casualty rate) could be enormous. The risk to Earth’s inhabitants is therefore finite, warranting action to improve and expand our ability to detect Earth- orbit-crossing objects and to analyze and predict their orbits. It would also be useful to explore methods and technologies for deflecting or destroying any such objects that are predicted to impact the Earth and to alter their orbits sufficiently to preclude impact. To begin the process of implementing such action, appropriate experts, both civil and military, should be tasked to formulate specific programs designed to address the issues involved. INTRODUCTION On March 23, 1989, an asteroid bigger than an aircraft carrier, traveling at 46,000 miles per hour, passed through Earth's orbit less than 400,000 miles away. Our planet had been at that point only six hours earlier.
  • 5 the Orbit of Mercury

    5 the Orbit of Mercury

    Name: Date: 5 The Orbit of Mercury Of the five planets known since ancient times (Mercury, Venus, Mars, Jupiter, and Saturn), Mercury is the most difficult to see. In fact, of the 6 billion people on the planet Earth it is likely that fewer than 1,000,000 (0.0002%) have knowingly seen the planet Mercury. The reason for this is that Mercury orbits very close to the Sun, about one third of the Earth’s average distance. Therefore it is always located very near the Sun, and can only be seen for short intervals soon after sunset, or just before sunrise. It is a testament to how carefully the ancient peoples watched the sky that Mercury was known at least as far back as 3,000 BC. In Roman mythology Mercury was a son of Jupiter, and was the god of trade and commerce. He was also the messenger of the gods, being “fleet of foot”, and commonly depicted as having winged sandals. Why this god was associated with the planet Mercury is obvious: Mercury moves very quickly in its orbit around the Sun, and is only visible for a very short time during each orbit. In fact, Mercury has the shortest orbital period (“year”) of any of the planets. You will determine Mercury’s orbital period in this lab. [Note: it is very helpful for this lab exercise to review Lab #1, section 1.5.] Goals: to learn about planetary orbits • Materials: a protractor, a straight edge, a pencil and calculator • Mercury and Venus are called “inferior” planets because their orbits are interior to that of the Earth.
  • O Lunar and Planetary Institute a Provided by the NASA

    O Lunar and Planetary Institute a Provided by the NASA

    SEARCHING FOR COMET CORES AMONG APOLLO/AMOR ASTEROIDS. C. A. Wood, SN4INASA Johnson Space Center, Houston, TX 77058 Other than occasional comets, Apollo and hor asteroids (AIA) approach the Earth more closely than any other celestial bodies, and hence are likely contributors to the flux of meteorites. Be- cause dynamic lifetimes of A/A objects are only lo7-lo8 years they must be continually resupplied from a longer-lived source. Orbital dynamical considerations appear to dictate that comets mst supply the majority of A/A1s, but, assuming that meteorites do come from A/A1s, current models of meteorite origins preclude this possibility. This standoff, between theories and models, has con- tinued for nearly 30 years, but sufficient data on A/A objects themselves are now available to con- sider the likelihood of a canetary or asteroidal origin for individual Earth-approaching objects. How to Identify Cometary Cores: Based upon previous discussions, extinct comets in A/A orbits are likely to be distinguishable from objects which escaped from the main asteroid belt by both physical and orbital characteristics (e.g., 1). Shape: Anders (2) argued that small objects such as Icarus (dia -1 km) could not maintain spherical shapes against collisional destruction if they had spent most of the last 4.5 b.y. in the asteroid belt. Collisional fragmentation would be much less likely in the Oort cloud, thus spheric- ity can be interpreted as evidence for a cometary origin of A/A objects. This criteria ignores the splitting of comets, which has only been observed in three shortperiod comets (13).
  • Asteroid Regolith Weathering: a Large-Scale Observational Investigation

    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.
  • Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa

    Deep Space Chronicle Deep Space Chronicle: a Chronology of Deep Space and Planetary Probes, 1958–2000 | Asifa

    dsc_cover (Converted)-1 8/6/02 10:33 AM Page 1 Deep Space Chronicle Deep Space Chronicle: A Chronology ofDeep Space and Planetary Probes, 1958–2000 |Asif A.Siddiqi National Aeronautics and Space Administration NASA SP-2002-4524 A Chronology of Deep Space and Planetary Probes 1958–2000 Asif A. Siddiqi NASA SP-2002-4524 Monographs in Aerospace History Number 24 dsc_cover (Converted)-1 8/6/02 10:33 AM Page 2 Cover photo: A montage of planetary images taken by Mariner 10, the Mars Global Surveyor Orbiter, Voyager 1, and Voyager 2, all managed by the Jet Propulsion Laboratory in Pasadena, California. Included (from top to bottom) are images of Mercury, Venus, Earth (and Moon), Mars, Jupiter, Saturn, Uranus, and Neptune. The inner planets (Mercury, Venus, Earth and its Moon, and Mars) and the outer planets (Jupiter, Saturn, Uranus, and Neptune) are roughly to scale to each other. NASA SP-2002-4524 Deep Space Chronicle A Chronology of Deep Space and Planetary Probes 1958–2000 ASIF A. SIDDIQI Monographs in Aerospace History Number 24 June 2002 National Aeronautics and Space Administration Office of External Relations NASA History Office Washington, DC 20546-0001 Library of Congress Cataloging-in-Publication Data Siddiqi, Asif A., 1966­ Deep space chronicle: a chronology of deep space and planetary probes, 1958-2000 / by Asif A. Siddiqi. p.cm. – (Monographs in aerospace history; no. 24) (NASA SP; 2002-4524) Includes bibliographical references and index. 1. Space flight—History—20th century. I. Title. II. Series. III. NASA SP; 4524 TL 790.S53 2002 629.4’1’0904—dc21 2001044012 Table of Contents Foreword by Roger D.
  • Asteroids + Comets

    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.