Interplanetary Dust PDF
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n^&l^n ASTRONOMY A ND ASTROPHYSICS LIBRARY LIBRARY Series Editors: I. Appenzeller, Heidelberg, Germany G. Börner, Garching, Germany M. Harwit, Washington, DC, USA R. Kippenhahn, Göttingen, Germany J. Lequeux, Paris, France P. A. Strittmatter, Tucson, AZ, USA V. Trimble, College Park, MD, and Irvine, CA, USA Springer-Verlag Berlin Heidelberg GmbH ONLINE LIBRARY Physics and Astronomy http://www.sprlnger.de/phys/ Eberhard Grün Bo Ä. S. Gustafson Stan Dermott Hugo Fechtig (Eds.) Interplanetary Dust With 242 Figures Including 4 Color Plates, and 46 Tables ;er Professor Eberhard Grün Professor Bo Ä. S. Gustafson Max-Planck-Institut für Kernphysik Department of Astronomy Saupfercheckweg 1 University of Florida 69117 Heidelberg, Germany Gainesville, FL 32611-2055, USA Professor Stan Dermott Professor Hugo Fechtig Department of Astronomy Max-Planck-Institut für Kernphysik University of Florida Saupfercheckweg 1 Gainesville, FL 32611-2055, USA 69117 Heidelberg, Germany Cover picture: A wedge of interplanetary dust. The dusk twilight sky (pink) towards th e northwest shows zodiacal light (blue), framed by the Pleiades (upper left), Come t Hale-Bopp (upper right), and Mercury in Aries (left of center above the horizon). This photograph was taken by Marco Fülle, 5 April 1997,18:50 UT, from the slopes of Stromboli (750 Meters above sea level), Sicily. ISSN 0941-7834 ISBN 978-3-642-62647-0 Library of Congress Cataloging-in-Publication Data applied for. Die Deutsche Bibliothek - CIP-Einheitsaufhahme Interplanetary dust: with 46 tables/Eberhard Grün ... (ed.). - Berlin; Heidelberg; New York; Barcelona; Hong Kong; London; Milan; Paris; Singapore; Tokyo: Springer, 2001 (Astronomy and astrophysics library) (Physics and astronomy online library) ISBN 978-3-642-62647-0 ISBN 978-3-642-56428-4 (eBook) DOI 10.1007/978-3-642-56428-4 This work is subject to copyright. All rights are reserved, whether the whole or part of the material is concerned, specifically the rights of translation, reprinting, reuse of illustrations, recitation, broadcasting, reproduction on microfilm or in any other way, and storage i n data banks. Duplication of this publication or parts thereof is permitted only under the provisions of the German Copyright Law of September 9,1965, in its current version, and permission for use must always be obtained from Springer-Verlag. Violations are liable for prosecution unde r the German Copyright Law. http://www.springer.de © Springer-Verlag Berlin Heidelberg 2001 Originally published by Springer-Verlag Berlin Heidelberg New York in 2001 The use of general descriptive names, registered names, trademarks, etc. in this publication does not imply, even in the absence of a specific statement, that such names are exempt from the relevant protective laws and regulations and therefore free for general use. Typesetting: Camera-ready version from the authors/editors Cover design: design & production GmbH, Heidelberg Printed on acid-free paper SPIN: 10836746 55/3141/tr - 5 4 3 2 1 0 To the memory of Herbert A. Zook (1932-2001 ) A scientist who inspired many chapters of the inter planetary d list story. Preface Conceived more than six years ago, this book took much effort to develop, and several updates in parts of the book became necessary because significant ad vances in the field of Interplanetary Dust had occurred. Now, at the beginning of the new millennium, this book provides up-to-date coverage of all major aspects of dust in the Solar System. The volume is conceived as a source book for researchers in the field as well as a graduate-level textbook. In order to achieve the highest standard the individual chapters are written by experts in the field, preserving the somewhat different style and language of the sub-topic. The book follows the comprehensive review of the "Cosmic Dust" field assembled by Tony McDonnell more than 20 years ago. That book covered dust in its various physical appearances as the common theme, but it described phenomena that appeared rather unrelated. The topics ranged from zodiacal light over lunar craters to dust particles collected in the atmosphere, from interstellar dust to comets, and from dust dynamics to laboratory simulation of dusty phenomena. Twenty years later, the field has matured far enough to warrant a new presentation in the form of a comprehensive review. Again, four major sub fields are at the center of the book: astronomical observations of dust in the Solar System and beyond, in situ measurements of dust in various locations of the planetary system, laboratory studies of interplanetary dust and of dusty phenomena, and theoretical investigations. However, this time, the field has become more integrated because of the many interrelations that have been developed between the sub-fields. Astronomical observations have extended the wavelength range from op tical to thermal infrared wavelengths for which dust is the major source. As a consequence, new information has been gathered about the structure of the interplanetary dust cloud, specifically in the outer Solar System. Dust around the Earth and other planets provides analogs to the interplanetary dust cloud where interrelationships between sources, sinks and dynamical effects can be studied more closely. New sophisticated instruments have been developed that provide in situ compositional analyses of dust. Micro-analytic laboratory tools are available to analyze collected dust grains structurally and compositionally on nano- to micrometer scales. Multi-disciplinary campaigns have been orga nized to study time-critical cometary and meteor phenomena. Sophisticated laboratory studies together with advanced theoretical developments provide the basis for the interpretation of astrophysical observations of dust. The description of the interplanetary dust cloud has evolved to synthetic models PREFACE Vlll representing a variety of observations, and even evolutionary models of compo nents of the zodiacal cloud are being developed. The discovery of interstellar grains traversing the planetary system and the detection of dust clouds around other stars opens the door to a whole new look at the Solar System dust cloud and beyond. However, the field is far from being complete. Despite the great advances made in recent years in the understanding of the interplanetary dust environ ment, there remain many important questions to be answered. Starting close to the Sun, nature separates meteoroid material according to its volatility. Anal ysis of the spatial distribution of matter close to the Sun will immediately give us information on the volatility of their constituents. Closer to home, the dust environment of the Earth is of interest, because mankind is affecting this environment due to our space activities. However, also the natural dust environment is of technological and scientific interest. Hazards from meteor streams (like the Leonids) will require continuous atten tion. Meteoroids that pass the Earth are of scientific interest because they are messengers from distant worlds, like asteroids, comets and even interstellar space. Once we know where dust grains originate from, compositional analysis of grains can tell us many things about these worlds. Therefore, the goal of such dust studies is to identify the sources of dust particles together with their in-depth analysis. The future of dust measurements in Earth orbit lies in three areas: (1) environmental monitoring; (2) use of dust telescopes to separate and analyze dust populations of different origin; and (3) collection and sample return of dust from various sources for in-depth analysis in laboratories. Enhanced dust densities in the Martian environment have long been sus pected. The comparison of future dust observations at Mars with those in the dusty rings of Saturn and the other giant planets will tell us what effects solar radiation pressure (strongest at Mars) and planetary magnetospheres (negligi ble at Mars) have. In addition, during a future human colonization of Mars, dust from the Martian satellites may play a similar hazardous role as space debris in the Earth environment. Analysis of particulates from comet Halley brought us new and important information that has relevance to the understanding of the formation of our planetary system. Currently the Stardust mission is on its way to analyze, collect and return dust from comet Tempel 2. This will give us a second example from the large variety of comets. It is the analysis of this variety that will tell us about the spatial and compositional variations in the protoplanetary nebula through the comets that may have sampled different regions of this nebula. The satellite and ring systems of the outer planets are models for the early Solar System with satellites and ring particles in intimate interactions. While Saturn's ring system is of high complexity, the rings of Jupiter, Uranus and Neptune show other features that have not yet been found elsewhere. The Pluto-Charon system may have rings with yet other features. To understand the common characteristics of all these rings and the reasons why they are so different requires detailed measurements of the rings and their environments. PREFACE ix Detection of Edgeworth-Kuiper belt objects (EKOs) of up to a few hundred kilometers diameter confirmed the existence of objects outside the planetary system. Mutual collisions among EKOs as well as impacts of interstellar grains generate dust locally. The action of the Poynting-Robertson effect together with resonances with the outer giant planets, interaction with the solar wind and neutral interstellar gas, may have lead to radial and azimuthal structure of the distribution of dust at the edge of the planetary system. The detection of infrared excess at main sequence stars started renewed interest in the outer extensions of our own Solar System dust cloud. Especially, the observation of dust disks around (3 Pictoris stimulated this interest. Observations of the Edgeworth-Kuiper dust belt in our Solar System can, therefore, be used as a model for extra-solar dust clouds and can help to reveal information about other planetary systems. The effects of the solar cycle-dependent heliosphere reach into interstellar space, out to about 300 AU from the Sun where it interferes with the small (~ 0.1 11m) particles entering the heliosphere and modulates their flow. Their origin, however, may be different from that of bigger grains that are accessi ble in Earth orbit. We know that evolved stars continuously lose mass. This "stardust" provides the seeds for interstellar dust grains that grow in cool inter stellar clouds by accretion of atoms and molecules and by agglomeration. An unbiased look into this interstellar dust factory will provide us with information on processes that are difficult to quantify by astronomical observations alone. Therefore, in situ dust analysis will be an important method when automated probes leave our Solar System. This collection of problems demonstrates that dust analysis will remain an important topic of planetary and astrophysical research and it is hoped that this book will stimulate interest in the study of these challenging issues. Further developments, errata, and related web sites can be found at http://www.springer.de/books/errata/interplanetary-dust/· The book has benefited from the support of a large number of people, many of whom are acknowledged in the individual chapters. We thank the chapter au thors for their efforts, persistence, and dedication to this project. Assistance in the preparation of the book from Amara Graps, Dagmar Koch, Harald Kruger, Markus Landgraf, and Richard Moissl is acknowledged. The unrewarded help of chapter reviewers is greatly appreciated: Josh Colwell, Bruce Draine, Ger hard Drolshagen, Dan Durda, Priscilla Frisch, Mayo Greenberg, Bob Hawkes, Doug Hamilton, Martha Hanner, Mihaly Honinyi, Don Humes, Eduard Igen bergs, Jochen Kissel, Wolfgang Klock, Mark Matney, Michel Maurette, Tony McDonnell, Derral Mulholland, Klaus Paul, Jiri Svestka, Tony Tuzzolino and Iwan Williams. Heidelberg, Gainesville, April 2001 Eberhard Griin Bo Gustafson Stanley Dermott Hugo Fechtig Contents Color Plates XXI Contributors XXVll Historical Perspectives ............................................ 1 Hugo Fechtig, Christoph Leinert, Otto E. Berg I. Introductory Overview ....................................... 1 II. Early Reports on the Zodiacal Light .......................... 2 III. Zodiacal Light Observations Until the Beginning of the Space Age ............................................. 10 IV. After the Beginning of the Space Age ......................... 17 IV.A. Rise and Fall of the Earth's Dust Belt .................. 17 IV.B. Zodiacal Light Studied from Near-Earth Space.......... 26 V. Microcraters on Lunar Surface Samples and the Lunar Ejecta and Micrometeorite Experiment ........ 30 VI. Experiments on Satellites and Space Probes .................. 36 VII. Important Results of the Dust Experiments PIA/PUMA and DIDSY on the Missions GIOTTO and VeGa to Comet Halley. 43 VIII. Outlook ...................................................... 45 References ......................................................... 47 Optical and Thermal Properties of Interplanetary Dust 57 Anny-Chantal Levasseur-Regourd, Ingrid Mann, Rene Dumont, Martha S. Hanner I. Zodiacal Scattered Light ......................................... 57 LA. Historical Survey .......................................... 58 LB. Zodiacal Light Measurements .............................. 59 I.C. Main Trends in the Data................................... 60 I.D. Zodiacal Brightness from 1 AU ............................ 63 I.E. Zodiacal Polarisation from 1 AU ........................... 66 II. F-Corona Scattered Light ....................................... 67 II.A. Solar Corona Observations................................ 67 II.B. Brightness and Polarisation of the F-Corona ............... 69 III. Zodiacal and F -Coronal Thermal Emission ..................... 72 lILA. Thermal Emission Measurements ......................... 72 III.B. Zodiacal Thermal Emission from 1 AU ................... 73 III.C. Thermal Emission from the F-Corona .................... 74 IV. Local Scattering and Thermal Properties ....................... 76 Xli CONTENTS IV.A. Need for Inversion ....................................... 76 IV.B. Volume Scattering and Emitting Functions ............... 77 IV.C. Inversion with Homogeneity Assumption ................. 79 IV.D. Local Rigorous Inversion ................................. 79 IV.E. Local Inversion Through Mathematical Methods.......... 80 IV.F Models of the Near Infrared F-Corona ..................... 85 V. Conclusions and Perspectives. . . . . .. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 86 References ......................................................... 88 Cometary Dust .................................................... 95 Zdenek Sekanina, Martha S. Hanner, Elmar K. Jessberger, Marina N. Fomenkova I. Introduction ..................................................... 95 II. Dust Dynamical Properties ...................................... 96 II.A. Ejection and Motion of Dust Grains ....................... 96 II.B. Dust Features in Cometary Heads ......................... 101 II.C. Dust Tails and Their Structure. . . . . . . . . . . . . . . . . . . . . . . . . . . . 108 II.D. Dust in Periodic Comet Shoemaker-Levy 9 ................ 115 III. Dust Optical and Physical Properties ........................... 120 lILA. Thermal Emission ....................................... 120 III.B. Silicates ................................................. 127 III.C. Infrared Spectral Features of Hydrocarbons ............... 130 III.D. Scattering by Dust ....................................... 132 III.E. Icy Grains ............................................... 136 IV. Dust Chemical and Isotopic Composition....................... 137 IV.A. Facts from Ion Spectra ................................... 138 IV.B. Bulk Composition........................................ 143 IV.C. Mineralogical Composition............................... 144 V. The Future ..................................................... 145 References ......................................................... 147 Near Earth Environment......................................... 163 Tony McDonnell, Neil McBride, Simon F. Green, Paul R. Ratcliff, David J. Gardner, Andrew D. Griffiths I. Introduction ..................................................... 163 II. The Earth as a Target .......................................... 165 II.A. Natural Meteoroids ....................................... 165 II.B. Meteoroid Properties and Dynamics....................... 166 II.C. The Sporadic Background................................. 174 II.D. The Annual Meteor Showers .............................. 174 II.E. Atmospheric Effects ....................................... 181 III. Space Debris ................................................... 189 IV. Modelling Tools................................................ 193 IV.A. The Griin Interplanetary Dust Model at 1 AU ............ 193
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