DOCSLIB.ORG

The International Conference on Asteroids, Comets, Meteors 1991

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The International Conference on Asteroids, Comets, Meteors 1991 ABSTRACTS FOR THE INTERNATIONAL CONFERENCE ON ASTEROIDS, COMETS, METEORS 1991 !'4 " a_ .... t _!K_J-- L' ', I , 1 ]_'sl ,_ >.;i_r _cL:_ i_l I (Lu ,_ U n C _1 .: ', Flagstaff, Arizona June 24-28, 1991 Sponsored by Barringer Crater Company Lunar and Planetary Institute Lowell Observatory Meteor Crater Enterprises, Inc. National Aeronautics and Space Administration (NASA) Northern Arizona University U.S. Geological Survey ABSTRACTS FOR THE INTERNATIONAL CONFERENCE ON ASTEROIDS, COMETS, METEORS 1991 Flagstaff, Arizona June 24-28, 1991 Sponsored by Barringer Crater Company Lunar and Planetary Institute Lowell Observatory Meteor Crater Enterprises, Inc. National Aeronautics and Space Administration (NASA) Northern Arizona University U.S. Geological Survey Compiled in 1991 by Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058-4399 LPI Contribution No. 765 Compiled in 1991 by Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058-4399 Material in this volume may be copied without restraint for library, abstract service, educational or personal research purposes; however, republication of any paper or portion thereof requires the written permission of the authors as well as appropriate acknowledgment of this publication. The Lunar and Planetary Institute is operated by the Universities Space Research Association under Contract No. NASW-4574 with the National Aeronautics and Space Administration. PREFACE This volume contains abstracts that have been accepted for presentation at the International Conference on Asteroids, Comets, Meteors 1991 in Flagstaff, Arizona, June 24-28, 1991. All abstracts accepted as of May I0, 1991 are included in alphabetical order of first authors. No distinctions have been made between invited papers, contributed papers, and poster papers. Late abstracts, if any, will be provided at the time of registration. Responsible for the program are Michael A'Hearn, University of Maryland; Edward Bowell, Lowell Observatory," Clark Chapman, Planetary Science Institute; Michel Festou, Observatoire Midi-Pyrbnbes; Alan Harris, Jet Propulsion Laboratory; Pamela Jones, Lunar and Planetary Institute; and Eugene Shoemaker, U.S. Geological Survey, Flagstaff. Logistics and administrative support were provided by the Program Services Department at the Lunar and Planetary Institute. The abstract volume was prepared by the Publications Services Department at the Lunar and Planetary Institute. Table of Contents Evolutionary Effects in Cometary Chemical Abundances M. E A'Hearn, R. L. Millis, D. G. Schleicher, D. J. Osip, and P. V. Birch Imaging Small Bodies with the Faint-Object Camera R. Albrecht Qualitative Researches of Evolution of Outer Part of Asteroidal Belt E. V. Alfimova and I. A. Gerasimov Characterizing Water/Rock Interactions in Simulated Comet Nuclei via Calorimetry: Tool for In-Situ Science, Laboratory Analysis, and Sample Preservation J. H. Allton and J. L. Gooding About Distribution and Origin of the Peculiar Group of Sporadic Meteors V. V. Andreev Phobos and Deimos are Sources of Meteoroids V. V. Andreev and O. I. Belkovich From C/Mrkos to P/Halley: 30 Years of Cometary Spectroscopy C. Arpigny, E Dossin, A. Woszczyk, B. Donn, Z Rahe, and S. Wyckoff ROSETTA, the Comet Nucleus Sample Return Mission 6 A. Atzei and R. Mitchell Fragmentation and Density of Meteoroids 7 P. B. Babadzhanov P/Machholz 1986 VIII and Quadrantid Meteoroid Stream. Orbital Evolution and Interrelation P. B. Babadzhanov and Yu. V. Obrubov Radar Meteor Orbital Structure of Southern Hemisphere Cometary Dust Streams W. Z Baggaley and A. D. Taylor A Southern Hemisphere Radar Meteor Orbit Survey W. J. Baggaley, D. I. Steel, and A. D. Taylor Diffusion of Gas Through Porous Dust Layers Formed in Comet Simulation 10 Experiments (KOSI) M. Baguhl, E. Grfin, and H. Kohl On the Validity of Markov Chain Methods For Modelling of Orbital Evolution 11 P. Baille and D. Hamburger Some Experiments Relevant to the Formation of a Cometary Organic Crust 12 G. A. Baratta and G. Strazzulla Comets Formation and their Contribution to the Volatiles on the Terrestrial Planets 13 A. Bar-Nun Does Exist a "Natural Break" in the Spin Distribution of Small Asteroids? 14 A. Barucci, M. Di Martino, and M. Fulchignoni PRECEDING PAGE BLArqK NOT RLMED The Nature of 951 Gaspra 15 A. Barucci, M. Di Martino, M. Fulchignoni, C. De Sanctis, and A. Rotundi On the Possibility of Determining the Mass of Some Minor Planets of the Hipparcos Programme 16 A. Bec-Borsenberger Determination of Meteor Flux Density Distribution Over the Celestial Sphere 16 O. I. Belkovich, 77.K. Filimonova, and V. E Sidorov The S-Type Asteroid Controversy 17 J. E Bell Asteroids with Unusual Lightcurves: 14 Irene and 51 Nemausa 18 I. N. Belskaya and A. N. Dovgopol Low Cost Missions to Explore the Diversity of Near Earth Cometary Nuclei 18 M. J. S. Belton Distribution of Active Areas on the Nucleus of Comet P[ Halley: Evidence for Inhomogeneity 19 M. J. S. Belton, I_. H. Julian, and B. E. A. Mueller Simulated Families: A Test of Different Methods of Families Identification 19 P. Bendjoya, A. Cellino, C Froc_chlk, and V. Zappal_ The Use of the Wavelet Cluster Analysis for Asteroid Family Determination 2O Ph. Bendjoya, E, Slezak, and CI. Froesehl# Stochasticity of Comet P/Slaughter-Burnham 2O D. Behest and R. Gonczi Lifetime and Cratering Record for Gaspra: A Pre-Galileo Estimate 21 R. P. Binzel and N. Namiki Trojan, Hilda, and Cybele Asteroids: Are They Really More Elongated Than Main-Belt Objects? 22 R. P. Binzel and I_, M. Sauter Low-Pressure Clathrate-Hydrato Formation in Amorphous Astrophysical Ice Analogs 23 D. E Blake, L. J. Allamandola, S. Sandford, D. Hudgins, and E Freund Observations of OH in Comet Levy (1990c) with the Naneay Radio Telescope 24 D. Bockelbe-Morvan, P. Colom, J. Crovisier, E. Gbrard, and G. Bourgois Coma Imaging of Comet P/Brorsen-Metcalf at Calar Alto in Late July to Mid August 1989 25 H. Boehnhardt, E Vanysek, K. Birkle, and U. Hopp Modeling the Coma of 2060 Chiton 26 D. C Boice, I. Konno, S. A. Stern, and I_. E Huebner Chaotic Behavior of Comet Nuclei 27 E. Bois, P. Obert, and Cl. Froeschlk H20 + Structures in the Inner Plasma Tail of Comet Austin 28 T. Bonev, K. Jockers, and E. H. Geyer vi Initial Overview of Disconnection Events in Halley's Comet 1986 29 J. C Brandt, C E. Randall, and Y Yi Asteroid Classification with Five ECAS Colors 3O D. T. Britt and I._ A. Lebofsky Observations of the Velocity and Spatial Distributions of Hydrogen in Comets Austin and Levy 31 M. E. Brown and H. Spinrad Implementation of Moving-Target Programs 32 M. W. Buie CCD Photometry of 2060 Chiton, 1991 January 33 B. J. Buratti, R. L Marcialis, E. S. Howell, and M. C Nolan Chiron: Evidence for Historic Cometary Activity 34 S. J. Bus, E. Bowell, S. A. Stern, M. E A'Hearn The Dust Coma of Comet Austin (1989ci) 35 H. Campins, S. C Tegler, C M. Telesco, and C Benson The Size Distribution of Asteroids from IRAS Data 35 A. Cellino, P. Farinella, and V. Zappakt Gross-Fragmentation of Meteoroids and Bulk Density of Geminids from Photographic Fireball Records 36 Z. Ceplecha and R. E. McCrosky Why Use Space Telescope? 37 C R. Chapman Gaspra: The Scientific Issues 38 C R. Chapman and D. R. Davis The Lifetime of Binary Asteroids vs. Gravitational Encounters and Collisions 39 B. Chauvineau, P. Farinella, and E Mignard On the Effects of the Observational Selection in the Modern Discoveries of Asteroids 39 N. S. Chernykh The Triplet d3A-a3_'rand Asundi al3g+a3_rr Bands of the Neutral CO in the Comet Scorichenko-George (1989e 1) Spectrum 4O K. I. Churyumov Solar Activity Influence Upon the Light Curves of Comets P/Halley (1986 III) and P/Churyumov-Gerasimenko (1982 VIII) 4O K. I. Churyumov and V. S. Filonenko Dust and Gas Jets. Evidence for a Diffuse Source in Halley's Coma 41 J. Clairemidi, P. Rousselot, E Vernotte, and G. Moreels The Coma of Comet P/Schwassmann-Wachmann 1 42 A. I_, Cochran and W. D. Cochran Observations of Cometary Parent Molecules with the IRAM Radio Telescope 43 P. Colom, D. Despois, G. Paubert, D. Bockel_e-Morvan, and J. Crovisier v// The Appearance of the 7.4-day Periodic Variation in the Spatial Profiles of C2, CN, NH2 and O(ID) in Comet Halley 44 M. K Combi and U. Fink Radio Spectroscopy of Comets: Recent Results and Future Prospects 45 J. Crovisier The Great Asteroid Nomenclature Controversy of 1801 45 C. J. Cunningham The Minor Planet Index to Scientific Papers 46 C. Cunningham Orbital Evolution Studies of Asteroids Near the 4:1 Mean Motion Resonance With Jupiter 47 M. Dahlgren, G. Hahn, C-I. Lagerkvist, and M. Lundstrom Observations of Comet Levy 1990c in the [OI] 6300 A Line with an Imaging Fabry-Perot C. Debi-Prasad, K. Jockers, H. Rauer, and E. H. Geyer Interplanetary Magnetic Field Changes and Condensation in Comet Halley's Plasma Tail 48 M. Delva, H. Lichtenegger, and K. Schwingenschuh The Origin and Evolution of the Zodiacal Dust Cloud 49 S. E Dermott, D. Durda, R. S. Gomes, B. Ggstafson, S. Jayaraman, Y-L Xu, and P D. Nicholson A Photometric Survey of Outer Belt Asteroids 5O M. Di Martino, M. Gonano-Beurer, S. Mottola, and S. Neukum On the Stability of the Asteroidal Belt 51 C. Diner and V. Shkodrov A Search for CO (1 -> 0) Emission in Comet Austin (1989cl) 51 M. DiSanti, M. Mumma, S. Hoban, J. Lacy, and R. Parmar Cometary Progenitors for Saturn-like Ring Systems 52 I_ Dones Eruptive Cosmogony of Minor Bodies and Their Interrelations 53 E. M. Drobyshevski The Sizes and Shapes of (4) Vesta, (216) Kleopatra, and (381) Myrrha From Occultations Observed During January 1991 54 D.
Load more

Recommended publications
  • Copyrighted Material
    Index Abulfeda crater chain (Moon), 97 Aphrodite Terra (Venus), 142, 143, 144, 145, 146 Acheron Fossae (Mars), 165 Apohele asteroids, 353–354 Achilles asteroids, 351 Apollinaris Patera (Mars), 168 achondrite meteorites, 360 Apollo asteroids, 346, 353, 354, 361, 371 Acidalia Planitia (Mars), 164 Apollo program, 86, 96, 97, 101, 102, 108–109, 110, 361 Adams, John Couch, 298 Apollo 8, 96 Adonis, 371 Apollo 11, 94, 110 Adrastea, 238, 241 Apollo 12, 96, 110 Aegaeon, 263 Apollo 14, 93, 110 Africa, 63, 73, 143 Apollo 15, 100, 103, 104, 110 Akatsuki spacecraft (see Venus Climate Orbiter) Apollo 16, 59, 96, 102, 103, 110 Akna Montes (Venus), 142 Apollo 17, 95, 99, 100, 102, 103, 110 Alabama, 62 Apollodorus crater (Mercury), 127 Alba Patera (Mars), 167 Apollo Lunar Surface Experiments Package (ALSEP), 110 Aldrin, Edwin (Buzz), 94 Apophis, 354, 355 Alexandria, 69 Appalachian mountains (Earth), 74, 270 Alfvén, Hannes, 35 Aqua, 56 Alfvén waves, 35–36, 43, 49 Arabia Terra (Mars), 177, 191, 200 Algeria, 358 arachnoids (see Venus) ALH 84001, 201, 204–205 Archimedes crater (Moon), 93, 106 Allan Hills, 109, 201 Arctic, 62, 67, 84, 186, 229 Allende meteorite, 359, 360 Arden Corona (Miranda), 291 Allen Telescope Array, 409 Arecibo Observatory, 114, 144, 341, 379, 380, 408, 409 Alpha Regio (Venus), 144, 148, 149 Ares Vallis (Mars), 179, 180, 199 Alphonsus crater (Moon), 99, 102 Argentina, 408 Alps (Moon), 93 Argyre Basin (Mars), 161, 162, 163, 166, 186 Amalthea, 236–237, 238, 239, 241 Ariadaeus Rille (Moon), 100, 102 Amazonis Planitia (Mars), 161 COPYRIGHTED
    [Show full text]
  • Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar End
    N9 Spacewalch Discovery of Near-Earth Asteroids Tom Gehrele Lunar end Planetary Laboratory The University of Arizona Our overall scientific goal is to survey the solar system to completion -- that is, to find the various populations and to study their statistics, interrelations, and origins. The practical benefit to SERC is that we are finding Earth-approaching asteroids that are accessible for mining. Our system can detect Earth-approachers In the 1-km size range even when they are far away, and can detect smaller objects when they are moving rapidly past Earth. Until Spacewatch, the size range of 6 - 300 meters in diameter for the near-Earth asteroids was unexplored. This important region represents the transition between the meteorites and the larger observed near-Earth asteroids (Rabinowitz 1992). One of our Spacewatch discoveries, 1991 VG, may be representative of a new orbital class of object. If it is really a natural object, and not man-made, its orbital parameters are closer to those of the Earth than we have seen before; its delta V is the lowest of all objects known thus far (J. S. Lewis, personal communication 1992). We may expect new discoveries as we continue our surveying, with fine-tuning of the techniques. III-12 Introduction The data accumulated in the following tables are the result of continuing observation conducted as a part of the Spacewatch program. T. Gehrels is the Principal Investigator and also one of the three observers, with J.V. Scotti and D.L Rabinowitz, each observing six nights per month. R.S. McMillan has been Co-Principal Investigator of our CCD-scanning since its inception; he coordinates optical, mechanical, and electronic upgrades.
    [Show full text]
  • CAPTURE of TRANS-NEPTUNIAN PLANETESIMALS in the MAIN ASTEROID BELT David Vokrouhlický1, William F
    The Astronomical Journal, 152:39 (20pp), 2016 August doi:10.3847/0004-6256/152/2/39 © 2016. The American Astronomical Society. All rights reserved. CAPTURE OF TRANS-NEPTUNIAN PLANETESIMALS IN THE MAIN ASTEROID BELT David Vokrouhlický1, William F. Bottke2, and David Nesvorný2 1 Institute of Astronomy, Charles University, V Holešovičkách 2, CZ–18000 Prague 8, Czech Republic; [email protected] 2 Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302; [email protected], [email protected] Received 2016 February 9; accepted 2016 April 21; published 2016 July 26 ABSTRACT The orbital evolution of the giant planets after nebular gas was eliminated from the Solar System but before the planets reached their final configuration was driven by interactions with a vast sea of leftover planetesimals. Several variants of planetary migration with this kind of system architecture have been proposed. Here, we focus on a highly successful case, which assumes that there were once five planets in the outer Solar System in a stable configuration: Jupiter, Saturn, Uranus, Neptune, and a Neptune-like body. Beyond these planets existed a primordial disk containing thousands of Pluto-sized bodies, ∼50 million D > 100 km bodies, and a multitude of smaller bodies. This system eventually went through a dynamical instability that scattered the planetesimals and allowed the planets to encounter one another. The extra Neptune-like body was ejected via a Jupiter encounter, but not before it helped to populate stable niches with disk planetesimals across the Solar System. Here, we investigate how interactions between the fifth giant planet, Jupiter, and disk planetesimals helped to capture disk planetesimals into both the asteroid belt and first-order mean-motion resonances with Jupiter.
    [Show full text]
  • 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.
    [Show full text]
  • Amateur Observers Find an Asteroid's Moon
    Amateur Observers Find an Asteroid’s Moon By: Kelly Beatty | July 14, 2017 A team of amateurs observers, some armed with just 3-inch telescopes, have found that the main-belt asteroid 113 Amalthea probably has a small companion. Each year, amateur astronomers get worldwide predictions for hundreds of events during which a distant asteroid briefly occults (hides) a star. But some of these cover-ups — like the one involving asteroid 113 Amalthea last March 14th — are anticipated more eagerly than others. That date has been circled on Paul Maley's calendar for about 8 months. A retired NASA staffer and a key member of the International Occultation Timing Association, last year Maley started enlisting amateur observers in Texas to observe the occultation of a 10th-magnitude star by 13th-magnitude Amalthea. And all that planning paid off, because the observing team has discovered that this asteroid probably has a small satellite. It's a robust "probably." As detailed in the IAU's Electronic Telegram 4413, issued on July 12th, a "fence" of 10 observing sites spread across the occultation's predicted path yielded seven positive occultations and three "misses." One of those misses, by Sam Insana in Gila Bend, Arizona, fell between five positive occultation tracks to his north and two to his south. It's colored orange in the diagram below: These lines represent the projected paths of a 10th-magnitude star recorded by observers on March 14, 2017, as the star passed behind the asteroid Amalthea. The small brown circle just below the yellow oval correspond to the location of the asteroid's moon at the time.
    [Show full text]
  • Using Resources from Near-Earth Space
    USING RESOURCES FROM NEAR-EARTH SPACE JOHN S. LEWIS University of Arizona DAVIDS. McKAY NASA Johnson Space Center and BENTON C. CLARK Martin Marietta Civil Space & Communications The parts of the solar system that are most accessible from Earth (the Moon, the near­ Earth asteroids, and Mars and its moons) are rich in materials of great potential value to humanity. Immediate uses of these resources to manufacture propellants, structural metals, refractories, life-support fluids and glass can support future large-scale space acitivites. In the longterm, non-terrestrial sources of rare materials and energy may be of great importance here on Earth. I. INTRODUCTION Space activities have become so much a part of modem life that they are almost invisible. We are aware how important communications satellite relays are for inexpensive long-distance telephone calls and television news broadcast, and we see the color images of Earth's cloud cover in the weather reports on TV. But we are usually not aware that the commercial airplane in which we fly or the ferry we ride locates itself by using navigation satellites 12,000 miles above our heads. We may never hear that the Soviet Union launched several satellites each year dedicated to assessing the American, Canadian, and Argentine wheat crops to help plan their grain purchases. We may be even more astonished to know that the truck we just passed on the highway is being tracked by a satellite, or that the strategic balance between the great powers has long been monitored based on photographic, electronic imaging, radar, infrared, and signal monitoring from space.
    [Show full text]
  • Thermophysical Characteristics of the Large Main-Belt Asteroid (349
    Mon. Not. R. Astron. Soc. 000, 1–10 (2002) Printed 14 November 2018 (MN LATEX style file v2.2) Thermophysical characteristics of the large main-belt asteroid (349) Dembowska LiangLiang Yu1,2⋆, Bin Yang3,4, Jianghui Ji2 , Wing-Huen Ip1,5 1Space Science Institute, Macau University of Science and Technology, Taipa, Macau;† 2CAS Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China; 3European Southern Observatory, Alonso de C´ordova 3107, Vitacura, Casilla 19001, Santiago, Chile; 4Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China; 5Institute of Astronomy, National Central University, Jhongli, Taoyuan City 32001, Taiwan Received 2014 December 14; in original form 2014 December 30 ABSTRACT (349) Dembowska, a large, bright main-belt asteroid, has a fast rotation and oblique spin axis. It may have experienced partial melting and differentiation. We constrain Dembowska’s thermophysical properties, e.g., thermal inertia, roughness fraction, geometric albedo and ef- +12 2 0.5 1 +0.60 fective diameter within 3σ uncertainty of Γ = 20 7 Jm− s− K− , fr = 0.25 0.25, pv = +0.026 +7.5 − − 0.309 0.038, and Deff = 155.8 6.2 km, by utilizing the Advanced Thermophysical Model (ATPM)− to analyse four sets of− thermal infrared data obtained by IRAS, AKARI, WISE and Subaru/COMICS at different epochs. In addition, by modeling the thermal lightcurve ob- served by WISE, we obtain the rotational phases of each dataset. These rotationally resolved data do not reveal significant variations of thermal inertia and roughness across the surface, indicating the surface of Dembowska should be covered by a dusty regolith layer with few rocks or boulders.
    [Show full text]
  • (704) Interamnia from Its Occultations and Lightcurves
    International Journal of Astronomy and Astrophysics, 2014, 4, 91-118 Published Online March 2014 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2014.41010 A 3-D Shape Model of (704) Interamnia from Its Occultations and Lightcurves Isao Satō1*, Marc Buie2, Paul D. Maley3, Hiromi Hamanowa4, Akira Tsuchikawa5, David W. Dunham6 1Astronomical Society of Japan, Yamagata, Japan 2Southwest Research Institute, Boulder, USA 3International Occultation Timing Association, Houston, USA 4Hamanowa Astronomical Observatory, Fukushima, Japan 5Yanagida Astronomical Observatory, Ishikawa, Japan 6International Occultation Timing Association, Greenbelt, USA Email: *[email protected], [email protected], [email protected], [email protected], [email protected], [email protected] Received 9 November 2013; revised 9 December 2013; accepted 17 December 2013 Copyright © 2014 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract A 3-D shape model of the sixth largest of the main belt asteroids, (704) Interamnia, is presented. The model is reproduced from its two stellar occultation observations and six lightcurves between 1969 and 2011. The first stellar occultation was the occultation of TYC 234500183 on 1996 De- cember 17 observed from 13 sites in the USA. An elliptical cross section of (344.6 ± 9.6 km) × (306.2 ± 9.1 km), for position angle P = 73.4 ± 12.5˚ was fitted. The lightcurve around the occulta- tion shows that the peak-to-peak amplitude was 0.04 mag. and the occultation phase was just be- fore the minimum.
    [Show full text]
  • Observations from Orbiting Platforms 219
    Dotto et al.: Observations from Orbiting Platforms 219 Observations from Orbiting Platforms E. Dotto Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino M. A. Barucci Observatoire de Paris T. G. Müller Max-Planck-Institut für Extraterrestrische Physik and ISO Data Centre A. D. Storrs Towson University P. Tanga Istituto Nazionale di Astrofisica Osservatorio Astronomico di Torino and Observatoire de Nice Orbiting platforms provide the opportunity to observe asteroids without limitation by Earth’s atmosphere. Several Earth-orbiting observatories have been successfully operated in the last decade, obtaining unique results on asteroid physical properties. These include the high-resolu- tion mapping of the surface of 4 Vesta and the first spectra of asteroids in the far-infrared wave- length range. In the near future other space platforms and orbiting observatories are planned. Some of them are particularly promising for asteroid science and should considerably improve our knowledge of the dynamical and physical properties of asteroids. 1. INTRODUCTION 1800 asteroids. The results have been widely presented and discussed in the IRAS Minor Planet Survey (Tedesco et al., In the last few decades the use of space platforms has 1992) and the Supplemental IRAS Minor Planet Survey opened up new frontiers in the study of physical properties (Tedesco et al., 2002). This survey has been very important of asteroids by overcoming the limits imposed by Earth’s in the new assessment of the asteroid population: The aster- atmosphere and taking advantage of the use of new tech- oid taxonomy by Barucci et al. (1987), its recent extension nologies. (Fulchignoni et al., 2000), and an extended study of the size Earth-orbiting satellites have the advantage of observing distribution of main-belt asteroids (Cellino et al., 1991) are out of the terrestrial atmosphere; this allows them to be in just a few examples of the impact factor of this survey.
    [Show full text]
  • CURRICULUM VITAE, ALAN W. HARRIS Personal: Born
    CURRICULUM VITAE, ALAN W. HARRIS Personal: Born: August 3, 1944, Portland, OR Married: August 22, 1970, Rose Marie Children: W. Donald (b. 1974), David (b. 1976), Catherine (b 1981) Education: B.S. (1966) Caltech, Geophysics M.S. (1967) UCLA, Earth and Space Science PhD. (1975) UCLA, Earth and Space Science Dissertation: Dynamical Studies of Satellite Origin. Advisor: W.M. Kaula Employment: 1966-1967 Graduate Research Assistant, UCLA 1968-1970 Member of Tech. Staff, Space Division Rockwell International 1970-1971 Physics instructor, Santa Monica College 1970-1973 Physics Teacher, Immaculate Heart High School, Hollywood, CA 1973-1975 Graduate Research Assistant, UCLA 1974-1991 Member of Technical Staff, Jet Propulsion Laboratory 1991-1998 Senior Member of Technical Staff, Jet Propulsion Laboratory 1998-2002 Senior Research Scientist, Jet Propulsion Laboratory 2002-present Senior Research Scientist, Space Science Institute Appointments: 1976 Member of Faculty of NATO Advanced Study Institute on Origin of the Solar System, Newcastle upon Tyne 1977-1978 Guest Investigator, Hale Observatories 1978 Visiting Assoc. Prof. of Physics, University of Calif. at Santa Barbara 1978-1980 Executive Committee, Division on Dynamical Astronomy of AAS 1979 Visiting Assoc. Prof. of Earth and Space Science, UCLA 1980 Guest Investigator, Hale Observatories 1983-1984 Guest Investigator, Lowell Observatory 1983-1985 Lunar and Planetary Review Panel (NASA) 1983-1992 Supervisor, Earth and Planetary Physics Group, JPL 1984 Science W.G. for Voyager II Uranus/Neptune Encounters (JPL/NASA) 1984-present Advisor of students in Caltech Summer Undergraduate Research Fellowship Program 1984-1985 ESA/NASA Science Advisory Group for Primitive Bodies Missions 1985-1993 ESA/NASA Comet Nucleus Sample Return Science Definition Team (Deputy Chairman, U.S.
    [Show full text]
  • Orbital Stability Assessments of Satellites Orbiting Small Solar System Bodies a Case Study of Eros
    Delft University of Technology, Faculty of Aerospace Engineering Thesis report Orbital stability assessments of satellites orbiting Small Solar System Bodies A case study of Eros Author: Supervisor: Sjoerd Ruevekamp Jeroen Melman, MSc 1012150 August 17, 2009 Preface i Contents 1 Introduction 2 2 Small Solar System Bodies 4 2.1 Asteroids . .5 2.1.1 The Tholen classification . .5 2.1.2 Asteroid families and belts . .7 2.2 Comets . 11 3 Celestial Mechanics 12 3.1 Principles of astrodynamics . 12 3.2 Many-body problem . 13 3.3 Three-body problem . 13 3.3.1 Circular restricted three-body problem . 14 3.3.2 The equations of Hill . 16 3.4 Two-body problem . 17 3.4.1 Conic sections . 18 3.4.2 Elliptical orbits . 19 4 Asteroid shapes and gravity fields 21 4.1 Polyhedron Modelling . 21 4.1.1 Implementation . 23 4.2 Spherical Harmonics . 24 4.2.1 Implementation . 26 4.2.2 Implementation of the associated Legendre polynomials . 27 4.3 Triaxial Ellipsoids . 28 4.3.1 Implementation of method . 29 4.3.2 Validation . 30 5 Perturbing forces near asteroids 34 5.1 Third-body perturbations . 34 5.1.1 Implementation of the third-body perturbations . 36 5.2 Solar Radiation Pressure . 36 5.2.1 The effect of solar radiation pressure . 38 5.2.2 Implementation of the Solar Radiation Pressure . 40 6 About the stability disturbing effects near asteroids 42 ii CONTENTS 7 Integrators 44 7.1 Runge-Kutta Methods . 44 7.1.1 Runge-Kutta fourth-order integrator . 45 7.1.2 Runge-Kutta-Fehlberg Method .
    [Show full text]
  • In Pursuit of the GENUINE CHRISTIAN IMAGE
    In Pursuit of THE GENUINE CHRISTIAN IMAGE Erland Forsberg as a Lutheran Producer of Icons in the Fields of Culture and Religion Juha Malmisalo Academic dissertation To be publicly discussed, by permission of the Faculty of Theology of the University of Helsinki, in Auditorium XII in the Main Building of the University, on May 14, 2005, at 10 am. Helsinki 2005 1 In Pursuit of THE GENUINE CHRISTIAN IMAGE Erland Forsberg as a Lutheran Producer of Icons in the Fields of Culture and Religion Juha Malmisalo Helsinki 2005 2 ISBN 952-91-8539-1 (nid.) ISBN 952-10-2414-3 (PDF) University Printing House Helsinki 2005 3 Contents Abbreviations .......................................................................................................... 4 Abstract ................................................................................................................... 6 Preface ..................................................................................................................... 7 1. Encountering Peripheral Cultural Phenomena ......................................... 9 1.1. Forsberg’s Icon Painting in Art Sociological Analysis: Conceptual Issues and Selected Perspectives ............................................................ 9 1.2. An Adaptation of Bourdieu’s Theory of Cultural Fields .......................... 18 1.3. The Pictorial Source Material: Questions of Accessibility and Method .. 23 2. Attempts at a Field-Constitution ................................................................ 30 2.1. Educational, Social, and
    [Show full text]