From: Amara Graps (Amara.Graps@mpi-hd.mpg.de)
Date: Fri Jan 11 2002 - 12:39:22 MST
Dear Extropes,
Here is an electronic (PDF), version of my PhD thesis for
distribution, in case any of you are interested in dust from the
Jovian system.
Many many many thanks to the Spikester, i.e. Spike Jones, for his
eagle-eye and eagle-mind, proofing this and catching my missed commas,
quotes, parenthesis, minus signs, and much more.
Amara
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Rupertus Carola University of Heidelberg, Germany
Department of Natural Science and Mathematics
PhD Dissertation July 2001
Amara Lynn Graps
"Io Revealed in the Jovian Dust Streams"
PDF ungzipped (32Mb)
http://www.mpi-hd.mpg.de/dustgroup/~graps/grapsthesis.pdf
PDF gzipped (23Mb)
http://www.mpi-hd.mpg.de/dustgroup/~graps/grapsthesis.pdf.gz
(very) SHORT SUMMARY
The Jovian dust streams are high-speed bursts of submicron-sized
particles traveling in the same direction from a source in the Jovian
system. Since their discovery in 1992, they have been observed by
three spacecraft: Ulysses, Galileo and Cassini. The source of the
Jovian dust streams is dust from Io's volcanoes. The charged and
traveling dust stream particles have particular signatures in
frequency space and in real space. The frequency-transformed Galileo
dust stream measurements show different signatures, varying
orbit-to-orbit during Galileo's first 29 orbits around Jupiter.
Time-frequency analysis demonstrates that Io is a localized source of
charged dust particles. Aspects of the particles' dynamics can be seen
in the December 2000 joint Galileo-Cassini dust stream measurements.
To match the travel times, the smallest dust particles could have the
following range of parameters: radius: 6 nm, density: 1.35--1.75g/cm^3,
sulfur charging conditions, which produce dust stream speeds:
220\450 km/s (Galileo\Cassini) and charge potentials: 5.5\6.3V
(Galileo\Cassini).
CONTENTS
1: Introduction {1}
1.1 Why Dust? {1}
1.2 Jovian Dust Streams History {2}
1.3 Thesis Statement {6}
2: In-Situ Measurements {9}
2.1 Dust Instruments {9}
2.2 Detection of Jovian Dust Streams {10}
2.3 Jupiter Millennium Mission {14}
3: Jovian Dust Streams as Frequencies {17}
3.1 Why Frequency Analysis? {17}
3.2 Methods of Time-frequency analysis {17}
3.3 Frequency-transformed Galileo Data {20}
4: Modeling {37}
4.1 Jupiter's Magnetic Field {37}
4.2 Jupiter's Plasma {45}
4.3 Torus-Magnetosphere Coupling {50}
4.4 Dust Particle Densities {51}
4.5 Dust Particle Optical Properties {51}
5: Charging {57}
5.1 Charging Processes {57}
5.2 Equilibrium Potential & Charging Times {64}
5.3 Dominant Currents {67}
5.4 Cassini-Galileo Joint Measurements Currents {67}
6: Dynamics {73}
6.1 Charged Particle Forces {73}
6.2 Ejection from the Jovian Magnetosphere {75}
6.3 Traveling SO_x Dust Particle Forces {84}
6.4 Dust Velocities vs. Distance {87}
6.5 Material Property Explorations {93}
7: Synopsis {99}
8: Going Further {103}
8.1 Ulysses Time-Freq Analysis {103}
8.2 Particle's Trajectory Errors {103}
8.3 A More Appropriate Magnetic Field {105}
Bibliography {107}
Appendices
A: Periodogram Derivation {113}
B: Frequency-Transformed Galileo Data {115}
C: Corotation {123}
C.1 Derivation of the Corotation Electric Field {123}
C.2 Derivation of the Magnetosphere Boundary {125}
D: Field Emission and Electrostatic Disruption {127}
List of Figures {128}
List of Tables {130}
Acknowledgements {131}
--
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Amara Graps, PhD | Max-Planck-Institut fuer Kernphysik
Heidelberg Cosmic Dust Group | Saupfercheckweg 1
+49-6221-516-543 | 69117 Heidelberg, GERMANY
Amara.Graps@mpi-hd.mpg.de * http://www.mpi-hd.mpg.de/dustgroup/~graps
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"Never fight an inanimate object." - P. J. O'Rourke
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