The stable magnetic field

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Table of contents

1 Introduction 
1.0.1 Layout of thesis
2 Mercury: History and context 
2.1 The Planet Mercury
2.1.1 Orbital parameters
2.1.2 Internal structure, the magnetic field and magnetosphere
2.1.3 Surface
2.1.4 Exosphere
2.2 History and science: Ancient
2.3 Science: In modern times
2.3.1 Early Optical observations
2.3.2 Modern ground-based observations
2.3.3 Missions
2.3.4 Modelling the exosphere of Mercury: a brief history
2.4 Summary
3 SPICAV: Differentiate ultraviolet signatures 
3.1 Stellar occultations and calibrations of the SPICAM and SPICAV instruments
3.2 The UV spectrometers on board the Mars Express and the Venus Express missions
3.2.1 General overview of the instruments
3.2.2 SPICAM and SPICAV datasets
3.3 Star calibration
3.3.1 Theoretical background
3.3.2 Observation of intensity decrease in high wavelengths
3.4 Summary
4 PHEBUS: Instrumentation for a harsh environment 
4.1 Radiometric Modelling and Scientific Performance of PHEBUS
4.2 Theoretical background
4.2.1 Instrument
4.2.2 Objectives and demands on the instrument
4.2.3 Sources
4.2.4 Optical layout
4.2.5 Photometric assessment and spectral resolution
4.3 Theoretical Results
4.3.1 Radiometric modelling of star spectra
4.3.2 In-flight calibrations of stars
4.4 Summary
5 Modelling Mercury’s hydrogen exosphere 
5.1 Introduction
5.2 SECTION I: The physics behind
5.2.1 Definitions and basic exospheric theory
5.2.2 Mechanisms of ejection from the surface: Maxwell-Boltzmann distributions
5.2.3 Temperature mapping
5.2.4 Ballistic motion of particles in the exosphere and external conditions
5.2.5 Sources of hydrogen at Mercury: Thermal processes
5.2.6 Sinks of hydrogen at Mercury: Ionisation
5.2.7 Deriving emission line brightness: radiative transfer and optical thickness (with Jean-Yves Chaufray)
5.3 SECTION II: Monte Carlo model
5.3.1 Coordinate system
5.3.2 Flow of program
5.3.3 Time evolution of the particle
5.3.4 Euler solution to ballistic motion
5.3.5 Outputs
5.4 Validation
5.4.1 Convergence criteria
5.4.2 Chamberlain
5.4.3 Thermalisation at surface
5.5 Sensitivity study
5.5.1 MB and MBF Velocity distribution functions
5.5.2 Accommodation coefficient
5.5.3 Source regions
5.5.4 Comparison to Mariner 10 data
5.5.5 Prediction of expected PHEBUS signal
5.6 Summary
6 Conclusion