Io Revealed in the Jovian Dust Streams

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"

(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).
[Ascii Synopsis, and University archive]

Dowload Full Text:
[PDF ungzipped (32Mb)]         [PDF gzipped (23Mb)] 
CONTENTS


Front Matter (PDF)
1:Introduction{1}
Chapt. 1 (PDF)
1.1     Why Dust?{1}
1.2	     Jovian Dust Streams History{2}
1.3	          Thesis Statement{6}
2:In-Situ Measurements{9}
Chapt. 2 (PDF)
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}
Chapt. 3 (PDF)
3.1     Why Frequency Analysis?{17}
3.2          Methods of Time-frequency analysis{17}
3.3	          Frequency-transformed Galileo Data{20}
4:Modeling	  {37}
Chapt. 4 (PDF)
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}
Chapt. 5 (PDF)
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}
Chapt. 6 (PDF)
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}
Chapt. 7 (PDF)
8:Going Further		    {103}
Chapt. 8 (PDF)
8.1     Ulysses Time-Freq Analysis{103}
8.2	     Particle's Trajectory Errors{103}
8.3	          A More Appropriate Magnetic Field{105}
Bibliography	  {107}
Biblio (PDF)
Appendices
A:Periodogram Derivation{113}
B:Frequency-Transformed Galileo Data{115}
C:Corotation{123}
C.1Derivation 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}
Back Matter and Acknowledgement. (PDF)
List of Tables{130}
Acknowledgements{131}

Conference Talks / Papers:

Graps' Main page Cosmic Dust Group

Last Modified by Amara Graps on 30 May 2002.