Table Of Contentn^&l^n ASTRONOMY A ND
ASTROPHYSICS LIBRARY
LIBRARY
Series Editors: I. Appenzeller, Heidelberg, Germany
G. Börner, Garching, Germany
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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
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© Springer-Verlag Berlin Heidelberg 2001
Originally published by Springer-Verlag Berlin Heidelberg New York in 2001
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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
