Investigation of the Magnetosphere of Ganymede with Galileo's Energetic Particle Detector

Ph.D. dissertation by Shawn M. Stone, University of Kansas, 1999.

Copyright 1999 by Shawn M. Stone.  Used with permission.

Chapter 4. Magnetic Field Models

The magnetic fields used in the simulation are the topic of this chapter. A basic review on the origins of these models is discussed. By the end of the chapter there will be two magnetic field models for the magnetic field environment in the vicinity of Ganymede for evaluation. The first, labeled here as model 1 (M1), comprises the dipole model proposed by Kivelson et al. [1996], a dipole field intrinsic to Ganymede and a background field of Jupiter based on the O6 model of Connerney [1993] and the hinged magnetodisk model of Khurana [1997]. The second model is one that is constructed from an internal multipole model for Ganymede, the background field of Jupiter as measured by the magnetometer prior to entry into the magnetosphere, and a magnetopause and tail field configuration using the external multipole model formalism of Choe and Beard [1973, 1974]. This second model is labeled throughout this work as model 2 (M2).

• 4.1 Offset Tilted Dipole Models
• 4.2 Spherical Harmonic Models
• 4.3 Modeling of External Sources: Magnetopause and Tail Fields
• 4.4 The O6 Multipole Model of the Jovian Internal Field
• 4.5 The Magnetodisk Current Sheet: Vector Potential Model
• 4.6 The Magnetodisk Current Sheet: Euler Potential Model
• 4.7 Ganymede Field: Construction of Model 1
• 4.8 Ganymede Field: Construction of Model 2
• 4.9 The Divergence of Magnetic Field in Models M1 and M2
• 4.10 Using the EPD Instrument to Check for Aberration of the Plasma Direction

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