The Complex History of Trojan Asteroids

Total Page:16

File Type:pdf, Size:1020Kb

The Complex History of Trojan Asteroids Emery J. P., Marzari F., Morbidelli A., French L. M., and Grav T. (2015) The complex history of Trojan asteroids. In Asteroids IV (P. Michel et al., eds.), pp. 203–220. Univ. of Arizona, Tucson, DOI: 10.2458/azu_uapress_9780816532131-ch011. The Complex History of Trojan Asteroids Joshua P. Emery University of Tennessee Francesco Marzari Università di Padova Alessandro Morbidelli Lagrange Laboratory, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS Linda M. French Illinois Wesleyan University Tommy Grav Planetary Science Institute The Trojan asteroids, orbiting the Sun in Jupiter’s stable Lagrange points, provide a unique perspective on the history of our solar system. As a large population of small bodies, they record important gravitational interactions in the dynamical evolution of the solar system. As primi- tive bodies, their compositions and physical properties provide windows into the conditions in the solar nebula in the region in which they formed. In the past decade, significant advances have been made in understanding their physical properties, and there has been a revolution in thinking about the origin of Trojans. The ice and organics generally presumed to be a signifi- cant part of Trojan composition have yet to be detected directly, although the low density of the binary system Patroclus (and possibly low density of the binary/moonlet system Hektor) is consistent with an interior ice component. By contrast, fine-grained silicates that appear to be similar to cometary silicates in composition have been detected, and a color bimodality may indicate distinct compositional groups among the Trojans. Whereas Trojans had traditionally been thought to have formed near 5 AU, a new paradigm has developed in which the Trojans formed in the proto-Kuiper belt, and were scattered inward and captured in the Trojan swarms as a result of resonant interactions of the giant planets. Whereas the orbital and population distributions of current Trojans are consistent with this origin scenario, there are significant differences between current physical properties of Trojans and those of Kuiper belt objects. These differences may be indicative of surface modification due to the inward migration of objects that became the Trojans, but understanding of appropriate modification mechanisms is poor and would benefit from additional laboratory studies. Many open questions about this intriguing population remain, and the future promises significant strides in our understanding of Trojans. The time is ripe for a spacecraft mission to the Trojans, to transform these objects into geologic worlds that can be studied in detail to unravel their complex history. 1. INTRODUCTION the term Trojan eventually came to be used for any object trapped in the L4 or L5 region of any body. Nevertheless, only Originally considered as simply an extension of the main Jupiter Trojans are named from the Iliad, and when used with- belt, Trojan asteroids have become recognized as a large out a designator, “Trojan” refers either specifically to Jupiter and important population of small bodies. Trojans share Ju- Trojans or sometimes to the collection of all bodies in stable piter’s orbit around the Sun, residing in the L4 and L5 stable Lagrange points. Several other solar system bodies also sup- Lagrange regions. Leading and trailing Jupiter by 60°, these port stable Trojan populations, including Mars, Neptune, and are regions of stable equilibrium in the Sun-Jupiter-asteroid two satellites of Saturn (Tethys and Dione). The populations three-body gravitational system. The moniker “Trojan” is coorbiting with Mars and the two saturnian moons appear to an artifact of history — the first three objects discovered in be quite small, but Neptune’s family of Trojans is thought Jupiter’s Lagrange regions were named after heroes from the to be extensive (e.g., Sheppard and Trujillo, 2010). Planets Iliad. The naming convention stuck for Jupiter’s swarms, and can destabilize each other’s Lagrange regions. For instance, 203 204 Asteroids IV Saturn and Uranus do not have stable Trojan populations to explain the capture of Trojans settled on two potential because the other planets perturb the orbits on timescales that mechanisms as most likely: gas drag in the early nebula are short relative to the age of the solar system. The Jupiter (e.g., Peale, 1993) and capture during the growth of Jupiter Trojans, which are the focus of this chapter, are estimated (Marzari and Scholl, 1998a). Both mechanisms predict that to be nearly as populous as the main belt and have stability the present-day Trojans formed in the middle of the solar timescales that exceed the age of the solar system. nebula, near where they currently reside. Since there is no The history of the exploration of Trojan asteroids begins other reservoir of material available for study from this with Max Wolf, who, in the late nineteenth century, was region, the Trojans would, in this case, be an exciting win- the first to turn to wide-field astrophotography for asteroid dow into the conditions of the solar nebula near the snow discovery (Tenn, 1994). In early 1906 he detected an object line and near Jupiter’s formation region. However, neither near Jupiter’s L4 point, marking the first observational con- mechanism fully explains the current orbital properties of firmation of Lagrange’s three-body solution. An object was Trojans, particularly the high inclinations. detected near L5 later in 1906 by August Kopf, then another More recently, Morbidelli et al. (2005) proposed the near L4 in early 1907. These were later named (588) Achilles, capture of Trojans from the same population from which (617) Patroclus, and (624) Hektor, respectively (Nicholson, the Kuiper belt originated. The Nice model postulates that 1961). As physical studies of asteroids accelerated in the resonant interactions between Jupiter and Saturn temporarily 1970s and 1980s, the Trojans were included, and the first destabilize the orbits of Uranus and Neptune, which move sizes, albedos, rotation periods, and (visible wavelength) into the primordial Kuiper belt, scattering material widely spectra were published (e.g., Dunlap and Gehrels, 1969; Crui- across the solar system. In this framework, Jupiter’s primor- kshank, 1977; Hartmann and Cruikshank, 1978; Chapman dial Trojan population is lost and the Lagrange regions are and Gaffey, 1979). Gradie and Veverka (1980) established repopulated with this scattered Kuiper belt material. Dotto the paradigm, which is still commonly invoked, that the et al. (2008) include a description of this capture scenario low albedo and red spectral slopes are due to the presence and a discussion of the implications for Trojans. This mecha- of complex organic molecules on Trojan surfaces. By 1989, nism predicts that Trojans formed much farther out in the when the Asteroids II book was published, 157 Trojans were solar nebula (~20–35 AU). In this case, the Trojans would known, from which Shoemaker et al. (1989) estimated a total represent the most readily accessible repository of Kuiper population comparable to that of the main belt — an esti- belt material. In the years since those reviews, some aspects mate that still stands, to within a factor of a few. Discovery of the Nice model have been reworked, and refinements to and characterization accelerated rapidly for Trojans (as with this newer mechanism for Trojan capture have been made. all asteroids) through the end of the twentieth century, and Unraveling the complex history of the Trojans promises by the time of Asteroids III in 2002, 993 Trojans had been key insight into solar system evolution. As primitive objects, discovered. The number now stands at 6073. Trojan compositions provide direct indicators of the condi- Summarizing the state of knowledge of the physical tions of the nebula in the region(s) in which they formed. properties of Trojans at the turn of the twenty-first century, As a population of small bodies, Trojans act as unique Barucci et al. (2002) describe a population that is far more probes of the history, interaction, and physical processing homogeneous than the main belt, with uniformly low albedos of the solar system. In this chapter, we review the physical (pv ~ 0.03 to 0.07) and featureless, red-sloped spectra at vis- properties of Trojan asteroids and scenarios for their origin ible and near-infrared (VNIR) wavelengths (0.4–2.5 µm). A and evolution. We rely heavily on previous reviews for much later review by Dotto et al. (2008) reports additional spectral of the early work (Shoemaker et al., 1989; Barucci et al., observations, particularly of members of potential collisional 2002; Marzari et al., 2002a; Dotto et al., 2008; Slyusarev families (Dotto et al., 2006; Fornasier et al., 2007), the and Belskaya, 2014), focusing here on new observations and detection of signatures of fine-grained silicates (Emery et recent advances in the knowledge of Trojans. al., 2006), and the first bulk-density measurement Marchis( et al., 2006). From these properties and their locations at 2. PHYSICAL PROPERTIES 5.2 AU, Trojans have generally been inferred to contain a large fraction of H2O ice hidden from view by a refractory 2.1. Size Distribution mantle, and a higher abundance of complex organic mol- ecules than most main-belt asteroids (MBAs). Since those Most asteroid surveys are conducted in visible (reflected) reviews, significant strides have been made in the physical light, from which it is not possible to derive the size unless characterization of Trojans, which in turn provide new in- the albedo is known. Studies of size distributions, therefore, sights into the nature of these enigmatic bodies. often use absolute magnitude (Hv) as a proxy for size. For Marzari et al. (2002a) review models for the capture of a population like the Trojans, where the albedo distribution Trojans and the stability of the Lagrange regions that had is very uniform (see section 2.2), the Hv distribution should developed up to that point.
Recommended publications
  • Occultation Evidence for a Satellite of the Trojan Asteroid (911) Agamemnon Bradley Timerson1, John Brooks2, Steven Conard3, David W
    Occultation Evidence for a Satellite of the Trojan Asteroid (911) Agamemnon Bradley Timerson1, John Brooks2, Steven Conard3, David W. Dunham4, David Herald5, Alin Tolea6, Franck Marchis7 1. International Occultation Timing Association (IOTA), 623 Bell Rd., Newark, NY, USA, [email protected] 2. IOTA, Stephens City, VA, USA, [email protected] 3. IOTA, Gamber, MD, USA, [email protected] 4. IOTA, KinetX, Inc., and Moscow Institute of Electronics and Mathematics of Higher School of Economics, per. Trekhsvyatitelskiy B., dom 3, 109028, Moscow, Russia, [email protected] 5. IOTA, Murrumbateman, NSW, Australia, [email protected] 6. IOTA, Forest Glen, MD, USA, [email protected] 7. Carl Sagan Center at the SETI Institute, 189 Bernardo Av, Mountain View CA 94043, USA, [email protected] Corresponding author Franck Marchis Carl Sagan Center at the SETI Institute 189 Bernardo Av Mountain View CA 94043 USA [email protected] 1 Keywords: Asteroids, Binary Asteroids, Trojan Asteroids, Occultation Abstract: On 2012 January 19, observers in the northeastern United States of America observed an occultation of 8.0-mag HIP 41337 star by the Jupiter-Trojan (911) Agamemnon, including one video recorded with a 36cm telescope that shows a deep brief secondary occultation that is likely due to a satellite, of about 5 km (most likely 3 to 10 km) across, at 278 km ±5 km (0.0931″) from the asteroid’s center as projected in the plane of the sky. A satellite this small and this close to the asteroid could not be resolved in the available VLT adaptive optics observations of Agamemnon recorded in 2003.
    [Show full text]
  • Thermal-IR Spectral Analysis of Jupiter's Trojan Asteroids
    50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1238.pdf THERMAL-IR SPECTRAL ANALYSIS OF JUPITER’S TROJAN ASTEROIDS: DETECTING SILICATES. A. C. Martin1, J. P. Emery1, S. S. Lindsay2, 1The University of Tennessee Earth and Planetary Science Department, 1621 Cumberland Avenue, 602 Strong Hall, Knoxville TN, 37996, 2The University of Tennessee, De- partment of Physics, 1408 Circle Drive, Knoxville TN, 37996.. Introduction: Jupiter’s Trojan asteroids (hereafter (e.g., [11],[8]). Had Trojans and JFCs formed in the Trojans) populate Jupiter’s L4 and L5 Lagrange points. same region, Trojans should have fine-grained silicates The L4 and L5 points are dynamically stable over the in primarily amorphous phases. lifetime of the Solar System, and, therefore, Trojans Analysis of TIR spectra by [12] shows that the sur- could have resided in the L4 and L5 regions for nearly faces of three Trojans (624 Hektor, 1172 Aneas, and 911 4.5 Gyr [1]. However, it is still uncertain where the Tro- Agamemnon) have emissivity features similar to fine- jans formed and when they were captured. Asteroid or- grained silicates in comet comae. The TIR wavelength igins provide an effective means of constraining the region is beneficial for silicate mineralogy detection be- events that dynamically shaped the solar system. Tro- cause it contains fundamental Si-O molecular vibrations jans may help in determining the extent of radial mixing (stretching at 9 –12 µm and bending at 14 – 25 µm; that occurred during giant planet migration. [13]). Comets produce optically thin comae that result Trojans are thought to have formed in one of two in strong 10-µm emission features when comprised of locations: (1) in their current position (~5.2 AU), or (2) fine-grained (≤10 to 20 µm) dispersed silicates.
    [Show full text]
  • Asteroid Shape and Spin Statistics from Convex Models J
    Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen To cite this version: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen. Asteroid shape and spin statistics from convex models. Icarus, Elsevier, 2008, 198 (1), pp.91. 10.1016/j.icarus.2008.07.014. hal-00499092 HAL Id: hal-00499092 https://hal.archives-ouvertes.fr/hal-00499092 Submitted on 9 Jul 2010 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. Accepted Manuscript Asteroid shape and spin statistics from convex models J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen PII: S0019-1035(08)00283-2 DOI: 10.1016/j.icarus.2008.07.014 Reference: YICAR 8734 To appear in: Icarus Received date: 18 September 2007 Revised date: 3 July 2008 Accepted date: 7 July 2008 Please cite this article as: J. Torppa, V.-P. Hentunen, P. Pääkkönen, P. Kehusmaa, K. Muinonen, Asteroid shape and spin statistics from convex models, Icarus (2008), doi: 10.1016/j.icarus.2008.07.014 This is a PDF file of an unedited manuscript that has been accepted for publication.
    [Show full text]
  • Origin and Evolution of Trojan Asteroids 725
    Marzari et al.: Origin and Evolution of Trojan Asteroids 725 Origin and Evolution of Trojan Asteroids F. Marzari University of Padova, Italy H. Scholl Observatoire de Nice, France C. Murray University of London, England C. Lagerkvist Uppsala Astronomical Observatory, Sweden The regions around the L4 and L5 Lagrangian points of Jupiter are populated by two large swarms of asteroids called the Trojans. They may be as numerous as the main-belt asteroids and their dynamics is peculiar, involving a 1:1 resonance with Jupiter. Their origin probably dates back to the formation of Jupiter: the Trojan precursors were planetesimals orbiting close to the growing planet. Different mechanisms, including the mass growth of Jupiter, collisional diffusion, and gas drag friction, contributed to the capture of planetesimals in stable Trojan orbits before the final dispersal. The subsequent evolution of Trojan asteroids is the outcome of the joint action of different physical processes involving dynamical diffusion and excitation and collisional evolution. As a result, the present population is possibly different in both orbital and size distribution from the primordial one. No other significant population of Trojan aster- oids have been found so far around other planets, apart from six Trojans of Mars, whose origin and evolution are probably very different from the Trojans of Jupiter. 1. INTRODUCTION originate from the collisional disruption and subsequent reaccumulation of larger primordial bodies. As of May 2001, about 1000 asteroids had been classi- A basic understanding of why asteroids can cluster in fied as Jupiter Trojans (http://cfa-www.harvard.edu/cfa/ps/ the orbit of Jupiter was developed more than a century lists/JupiterTrojans.html), some of which had only been ob- before the first Trojan asteroid was discovered.
    [Show full text]
  • On the Accuracy of Restricted Three-Body Models for the Trojan Motion
    DISCRETE AND CONTINUOUS Website: http://AIMsciences.org DYNAMICAL SYSTEMS Volume 11, Number 4, December 2004 pp. 843{854 ON THE ACCURACY OF RESTRICTED THREE-BODY MODELS FOR THE TROJAN MOTION Frederic Gabern1, Angel` Jorba1 and Philippe Robutel2 Departament de Matem`aticaAplicada i An`alisi Universitat de Barcelona Gran Via 585, 08007 Barcelona, Spain1 Astronomie et Syst`emesDynamiques IMCCE-Observatoire de Paris 77 Av. Denfert-Rochereau, 75014 Paris, France2 Abstract. In this note we compare the frequencies of the motion of the Trojan asteroids in the Restricted Three-Body Problem (RTBP), the Elliptic Restricted Three-Body Problem (ERTBP) and the Outer Solar System (OSS) model. The RTBP and ERTBP are well-known academic models for the motion of these asteroids, and the OSS is the standard model used for realistic simulations. Our results are based on a systematic frequency analysis of the motion of these asteroids. The main conclusion is that both the RTBP and ERTBP are not very accurate models for the long-term dynamics, although the level of accuracy strongly depends on the selected asteroid. 1. Introduction. The Restricted Three-Body Problem models the motion of a particle under the gravitational attraction of two point masses following a (Keple- rian) solution of the two-body problem (a general reference is [17]). The goal of this note is to discuss the degree of accuracy of such a model to study the real motion of an asteroid moving near the Lagrangian points of the Sun-Jupiter system. To this end, we have considered two restricted three-body problems, namely: i) the Circular RTBP, in which Sun and Jupiter describe a circular orbit around their centre of mass, and ii) the Elliptic RTBP, in which Sun and Jupiter move on an elliptic orbit.
    [Show full text]
  • March 21–25, 2016
    FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk,
    [Show full text]
  • Structure and Composition of the Surfaces of Trojan Asteroids from Reflection and Emission Spectroscopy
    Lunar and Planetary Science XXXVII (2006) 2075.pdf STRUCTURE AND COMPOSITION OF THE SURFACES OF TROJAN ASTEROIDS FROM REFLECTION AND EMISSION SPECTROSCOPY. Joshua. P. Emery,1 Dale. P. Cruikshank,2 and Jeffrey Van Cleve3 1NASA Ames / SETI Institute ([email protected]), 2NASA Ames Research Center ([email protected]), 3 Ball Aerospace ([email protected]). Introduction: The orbits of Trojan asteroids (~5.2 AU – beyond the Main Belt) place them in the transi- 1.0 tion region between the rocky inner and icy outer Solar 0.9 1172 Aneas System. Most Trojans were traditionally thought to 0.8 have originated in this region [3], although other loca- 1.0 tions of origin are possible [e.g., 4,5,6]. Possible con- 0.9 nections between Trojans and other groups of objects 911 Agamemnon 0.8 (Jupiter family comets, irregular satellites, Centaurs, Emissivity KBOs) are also important, but only poorly understood 1.0 [4,6,7,9]. The compositions of Trojans thereby hold 0.9 624 Hektor important clues concerning conditions in this critical 0.8 transition region, and the solar nebula as a whole. We discuss emission and reflection spectra of three Trojans 10 15 20 25 30 35 Wavelength (µm) (624 Hektor, 911 Agamemnon, and 1172 Aneas) and implications for surface structure and composition. Figure 2. Mid-IR emissivity spectra of Trojans. Vis-NIR Reflectance Spectroscopy: Reflectance studies of Trojans in the visible and NIR (0.8 – 4.0 Analysis: The Trojans have a similar spectral shape µm) reveal dark surfaces with mild to very red spectral to some carbonaceous meteorites and fine-grained sili- slopes, but no distinct absorption features (Fig.
    [Show full text]
  • Astrocladistics of the Jovian Trojan Swarms
    MNRAS 000,1–26 (2020) Preprint 23 March 2021 Compiled using MNRAS LATEX style file v3.0 Astrocladistics of the Jovian Trojan Swarms Timothy R. Holt,1,2¢ Jonathan Horner,1 David Nesvorný,2 Rachel King,1 Marcel Popescu,3 Brad D. Carter,1 and Christopher C. E. Tylor,1 1Centre for Astrophysics, University of Southern Queensland, Toowoomba, QLD, Australia 2Department of Space Studies, Southwest Research Institute, Boulder, CO. USA. 3Astronomical Institute of the Romanian Academy, Bucharest, Romania. Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Jovian Trojans are two swarms of small objects that share Jupiter’s orbit, clustered around the leading and trailing Lagrange points, L4 and L5. In this work, we investigate the Jovian Trojan population using the technique of astrocladistics, an adaptation of the ‘tree of life’ approach used in biology. We combine colour data from WISE, SDSS, Gaia DR2 and MOVIS surveys with knowledge of the physical and orbital characteristics of the Trojans, to generate a classification tree composed of clans with distinctive characteristics. We identify 48 clans, indicating groups of objects that possibly share a common origin. Amongst these are several that contain members of the known collisional families, though our work identifies subtleties in that classification that bear future investigation. Our clans are often broken into subclans, and most can be grouped into 10 superclans, reflecting the hierarchical nature of the population. Outcomes from this project include the identification of several high priority objects for additional observations and as well as providing context for the objects to be visited by the forthcoming Lucy mission.
    [Show full text]
  • The Minor Planet Bulletin 44 (2017) 142
    THE MINOR PLANET BULLETIN OF THE MINOR PLANETS SECTION OF THE BULLETIN ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS VOLUME 44, NUMBER 2, A.D. 2017 APRIL-JUNE 87. 319 LEONA AND 341 CALIFORNIA – Lightcurves from all sessions are then composited with no TWO VERY SLOWLY ROTATING ASTEROIDS adjustment of instrumental magnitudes. A search should be made for possible tumbling behavior. This is revealed whenever Frederick Pilcher successive rotational cycles show significant variation, and Organ Mesa Observatory (G50) quantified with simultaneous 2 period software. In addition, it is 4438 Organ Mesa Loop useful to obtain a small number of all-night sessions for each Las Cruces, NM 88011 USA object near opposition to look for possible small amplitude short [email protected] period variations. Lorenzo Franco Observations to obtain the data used in this paper were made at the Balzaretto Observatory (A81) Organ Mesa Observatory with a 0.35-meter Meade LX200 GPS Rome, ITALY Schmidt-Cassegrain (SCT) and SBIG STL-1001E CCD. Exposures were 60 seconds, unguided, with a clear filter. All Petr Pravec measurements were calibrated from CMC15 r’ values to Cousins Astronomical Institute R magnitudes for solar colored field stars. Photometric Academy of Sciences of the Czech Republic measurement is with MPO Canopus software. To reduce the Fricova 1, CZ-25165 number of points on the lightcurves and make them easier to read, Ondrejov, CZECH REPUBLIC data points on all lightcurves constructed with MPO Canopus software have been binned in sets of 3 with a maximum time (Received: 2016 Dec 20) difference of 5 minutes between points in each bin.
    [Show full text]
  • VITA David Jewitt Address Dept. Earth, Planetary and Space
    VITA David Jewitt Address Dept. Earth, Planetary and Space Sciences, UCLA 595 Charles Young Drive East, Box 951567 Los Angeles, CA 90095-1567 [email protected], http://www2.ess.ucla.edu/~jewitt/ Education B. Sc. University College London 1979 M. S. California Institute of Technology 1980 Ph. D. California Institute of Technology 1983 Professional Experience Summer Student Royal Greenwich Observatory 1978 Anthony Fellowship California Institute of Technology 1979-1980 Research Assistant California Institute of Technology 1980-1983 Assistant Professor Massachusetts Institute of Technology 1983-1988 Associate Professor and Astronomer University of Hawaii 1988-1993 Professor and Astronomer University of Hawaii 1993-2009 Professor Dept. Earth, Planetary & Space Sciences, UCLA 2009- Inst. of Geophys & Planetary Physics, UCLA 2009-2011 Dept. Physics & Astronomy, UCLA 2010- Director Institute for Planets & Exoplanets, UCLA, 2011- Honors Regent's Medal, University of Hawaii 1994 Scientist of the Year, ARCS 1996 Exceptional Scientific Achievement Award, NASA 1996 Fellow of University College London 1998 Fellow of the American Academy of Arts and Sciences 2005 Fellow of the American Association for the Advancement of Science 2005 Member of the National Academy of Sciences 2005 National Observatory, Chinese Academy of Sciences, Honorary Professor 2006-2011 National Central University, Taiwan, Adjunct Professor 2007 The Shaw Prize for Astronomy 2012 The Kavli Prize for Astrophysics 2012 Foreign Member, Norwegian Academy of Sciences & Letters 2012 Research
    [Show full text]
  • Aas 14-267 Design of End-To-End Trojan Asteroid
    AAS 14-267 DESIGN OF END-TO-END TROJAN ASTEROID RENDEZVOUS TOURS INCORPORATING POTENTIAL SCIENTIFIC VALUE Jeffrey Stuart,∗ Kathleen Howell,y and Roby Wilsonz The Sun-Jupiter Trojan asteroids are celestial bodies of great scientific interest as well as potential natural assets offering mineral resources for long-term human exploration of the solar system. Previous investigations have addressed the auto- mated design of tours within the asteroid swarm and the transition of prospective tours to higher-fidelity, end-to-end trajectories. The current development incorpo- rates the route-finding Ant Colony Optimization (ACO) algorithm into the auto- mated tour generation procedure. Furthermore, the potential scientific merit of the target asteroids is incorporated such that encounters with higher value asteroids are preferentially incorporated during sequence creation. INTRODUCTION Near Earth Objects (NEOs) are currently under consideration for manned sample return mis- sions,1 while a recent NASA feasibility assessment concludes that a mission to the Trojan asteroids can be accomplished at a projected cost of less than $900M in fiscal year 2015 dollars.2 Tour concepts within asteroid swarms allow for a broad sampling of interesting target bodies either for scientific investigation or as potential resources to support deep-space human missions. However, the multitude of asteroids within the swarms necessitates the use of automated design algorithms if a large number of potential mission options are to be surveyed. Previously, a process to automatically and rapidly generate sample tours within the Sun-Jupiter L4 Trojan asteroid swarm with a mini- mum of human interaction has been developed.3 This scheme also enables the automated transition of tours of interest into fully optimized, end-to-end trajectories using a variety of electrical power sources.4,5 This investigation extends the automated algorithm to use ant colony optimization, a heuristic search algorithm, while simultaneously incorporating a relative ‘scientific importance’ ranking into tour construction and analysis.
    [Show full text]
  • Planetary Astronomy (Nasw-4266)
    N89- 16639 NATIONAL AERONAUTICS AN0 SPACE AOMlNlSTAATlON RESEARCH AND TECHNOLOGY RESUME TITLE PLANETARY ASTRONOMY (NASW-4266) PERFORMING ORGANIZATION Planetary Science Institute -_~ 2030 East Speedway, Suite 201 -- Tucson, Arizona 85719 INV EST1 G AZO R’S NAME Dr. Clark R. Chapman I OESCRIPTION la. Brief rtolcmenl on shatepy of inuerti#alion; b. Pro;mrr and accomplichmenlr of prior year; C. What will be occompllrhed fhu yew. 0s wrII as hoy-!_end why; and d. Summay bibllorraphy) a. s’trateqy: rhe above-referenced Flanefary Astronomy contract supports iivE 5enicr rese3Fchers at the Planetary Science Institute !firs. Campins, Chapman, Davis. Hartnann. and Weidenschilling! with some involvement of other staff members. The goal i; to use a varietv of observational techniques and instruments to redi-ice, interpret. 3nd syn+hesiro groundbased astronosicai data concerning the comets. asteroids, and other small bodies af the solar svstem in order to 5tiidv the compositinns, physical characteristics, popuiaticrn properties, and evolution of th~:? bodies. have performed a variety of programmatic tasks, as well, including Chapman’s cast chairmanship of the Planetary Astronomy MDWG. 1 : d. Summary biblioqraphy !attached) I 29 SUMMARY BIBLIOGRAPHY Ahrens. T.J., Campins. H. and 20 other authors (1987). Report of the Joint EStVNASA Science Definition Team, Rosetta: The Comet Nucleus Sample Return Mission. Campins, H.. Rieke. M.J.. and Rieke, G.H. (1988). An Infrared Color Gradient in the Inner Coma of Comet Halley, submitted to Icarus. Chapman, C.R. (1987). Distributions of Asteroid Compositional Types with Solar Distance, Body Diameter, and Family Membership, Meteoritics 22. 353-354. Chapman, C.R. (1987). The Asteroid Belt: Compositional Structure and Size Distributions, DPS abstract.
    [Show full text]