Earlier observations of kelvin-helmholtz

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Table of contents

I introduction 
1 interaction between solar wind and earth’s magnetosphere
1.1 Introduction
1.2 Solar wind and magnetospheric plasma regions
1.3 Magnetic Reconnection
1.3.1 Interplanetary Magnetic Field interaction with Geomagnetic field lines
1.4 Space Plasma Discontinuities
1.5 Plasma characteristic frequencies and scales in near Earth’s regions
1.6 Kelvin-Helmholtz and Rayleigh-Taylor Instabilities
1.6.1 Hydrodynamic case
1.6.2 Magnetohydrodynamic case
2 modelling kelvin-helmholtz instability using a two fluid code 
2.1 Numerical Simulations of Kelvin-Helmholtz instability
2.2 Two Fluid code
3 spacecraft observations in near earth’s space 
3.1 Earlier Observations of Kelvin-Helmholtz
3.2 Recent spacecraft missions
3.2.1 Cluster Mission
3.2.2 Geotail mission
3.2.3 ACE 2
3.3 Spacecraft data analysis methods
3.3.1 Minimum Variance Analysis
3.3.2 Timing method
3.3.3 DeHoffman Teller
3.3.4 The boundary normal coordinate system(LMN)
II turbulence in kelvin-helmholtz vortices
4 two fluid numerical simulation of turbulence in k-h vortices 
4.1 Initial plasma configuration
4.2 Turbulence Analysis
4.2.1 Hann window
4.2.2 Anisotropy
4.2.3 Current sheets and magnetic reconnection regions.
4.3 Discussion and Conclusions
III simulations of kelvin-helmholtz instability at the magnetopause initialized with experimental profiles
5 simulations based on satellites crossings of the magnetopause 
5.1 Selection of Cluster Data events
5.2 Event 2001-11-20
5.3 Velocity and density profile estimation
5.3.1 Cluster Crossing
5.3.2 Geotail data: Multi-crossings event
5.4 Simulation using experimental initial conditions
5.5 Simulations with higher velocity jump
5.6 Comparison with observational results
5.7 Discussion and Conclusions
IV conclusions and outlook 
V appendix 
a generalized ohm’s law
b the numerical code
Bibliography