In this thesis, a simple model of the stretched magnetic field lines in the nightside magnetotail was created. The nightside magnetosphere model contains four main regions: plasmasphere, plasma sheet, magnetic lobes, and low latitude boundary layers. The plasma sheet is split into three regions based on the shape of the closed field lines present: dipole plasma sheet, transition plasma sheet, and stretched plasma sheet (SPS). The SPS, the focus of this thesis, is split into two regions: disruption zones (DZs) and a central neutral sheet (NS). The shape of the stretched field lines contain four inflection points. The convex curvature regions form the DZs and the central concave curvature region forms the NS. The NS is split into two regions: outer neutral sheet (ONS) and inner neutral sheet (INS). Due to the reversal of the x-component of the magnetic field at the center line of the NS, the protons are magnetized in the ONS and "unmagnetized" in the INS. There are two main current systems in the SPS. The first is a double vortex current system consisting of eastward current in the DZs that closes westward in the NS. The second system is the NS field-aligned current (FAC) system. It is generated in the INS mainly by the earthward convective drift of the electrons while the "unmagnetized" protons have little convective drift and remain tailward of the electrons. This FAC system produces the pre-onset electron auroral arc during the growth phase of the substorm. A simple model of the stretched magnetic field lines was created in order to calculate the current systems present in the SPS. The simple model was based entirely upon the shape of the stretched field lines. It passed two physical tests, divergence of the magnetic field and limits at infinity, so it was used to calculate currents. The total current using Ampere's law and the curvature current was found. Both results agreed with the double vortex current system.

The thesis compares two different methods for tracking and moving field lines. The first method included tracing one field line and moving each individual vertex along its own path with path following. The second method was done by tracing new field lines and using linear interpolation to move the field lines. The results show that the first method was incapable of rendering the field lines correctly due to the complexity and non-linearity of Earth's magnetic field. While it was successful at animating the initial motion of the field lines, it was not able to demonstrate the field line's change in topology. The second method was able to solve this issue, correctly visualizing field lines in motion, including changes in topology. However, the solution is limited in that it assumes that the vector field is static, which is not the case. To improve the visualization, a method for tracing and tracking field lines through multiple datasets is required. / <p>Examensarbetet är utfört vid Institutionen för teknik och naturvetenskap (ITN) vid Tekniska fakulteten, Linköpings universitet</p>

The bow shock is formed due to the abrupt deceleration of the supersonic solar wind in front of the terrestrial magnetic field. The solar wind plasma and the Interplanetary Magnetic Field (IMF) are both compressed across the shock, and according to Ampère's law a current thus flows on the bow shock at all times. The Bow Shock Current (BSC) is suggested to play an important role in solar wind-magnetosphere coupling, but there is still an open debate about its closure path. For predominantly east-west IMF, the BSC has been suggested to close to Earth's high latitude ionosphere as Field-Aligned Currents (FACs). Since the bow shock is magnetically connected to the solar wind, it must do so via open field lines through the magnetosheath. For southwards IMF with a significant east-west component, the R0 FAC flows into the ionosphere in one hemisphere, and out of it in the other. The R0 current flows on open field lines, and is thus a potential candidate to close the BSC. While a few studies have already found evidence in favour of this idea, the majority have been based on simulations. Additional observational evidence is required to confirm these findings. We used OMNI data for the IMF at the bow shock, and Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE) data for the FACs, to make simultaneous observations of the IMF at the bow shock and the northern hemisphere FACs, including the R0 current. We successfully identified 15 events of southwards but predominantly east-west IMF (Bz&lt;0, |By|&gt;|Bz|) at the bow shock, for which the northern hemisphere R0 current could be observed both in the AMPERE and DMSP data. In each of these events, the R0 current was of the correct polarity to connect to the BSC. Moreover, using Defense Meteorological Satellite Program (DMSP) and Super Dual Auroral Radar Network (SuperDARN) data, we were able to verify that part of the R0 current was flowing on open field lines. Collectively, the 15 events presented here constitute an argument in favour of at least a partial BSC closure to Earth's high latitude ionosphere as R0 FACs, for predominantly east-west IMF. Additional investigation is required to reveal the details of BSC closure.

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The study investigated the impact of computer simulations on the teaching and learning of electromagnetism in grade 11. Electromagnetism is a section of the Physical Science curriculum. Two grade 11 classes in the Mgwenya circuit in Mpumalanga province of South Africa were used as a case study. Using a pre-test, post-test non-equivalent control group design, it was found that learners in the experimental group (n = 30) who were taught using the simulations achieved significantly higher scores on the post-test than learners in the control group (n = 35) who were taught using traditional teacher-centred teaching method; (t statistic = 3.582, df = 56, p<0.05). Learners were more active during the lessons, predicting, observing, discussing and explaining concepts. The use of simulations also provided support (scaffolding) that the learners need to enhance learning. The Hake’s normalized gain for the experimental group <g> = 0.32 compared to <g> = 0.18 for the control group confirmed conceptual improvement. Both teachers and learners indicated that they accept the use of computer simulations in teaching and learning of electromagnetism. / Science and Technology Education / M. Sc. (Mathematics, Science and Technology Education)

The study investigated the impact of computer simulations on the teaching and learning of electromagnetism in grade 11. Electromagnetism is a section of the Physical Science curriculum. Two grade 11 classes in the Mgwenya circuit in Mpumalanga province of South Africa were used as a case study. Using a pre-test, post-test non-equivalent control group design, it was found that learners in the experimental group (n = 30) who were taught using the simulations achieved significantly higher scores on the post-test than learners in the control group (n = 35) who were taught using traditional teacher-centred teaching method; (t statistic = 3.582, df = 56, p<0.05). Learners were more active during the lessons, predicting, observing, discussing and explaining concepts. The use of simulations also provided support (scaffolding) that the learners need to enhance learning. The Hake’s normalized gain for the experimental group <g> = 0.32 compared to <g> = 0.18 for the control group confirmed conceptual improvement. Both teachers and learners indicated that they accept the use of computer simulations in teaching and learning of electromagnetism. / Science and Technology Education / M. Sc. (Mathematics, Science and Technology Education)

Space weather is the field within the space sciences that studies how the Earths magnetosphere is influenced by the Sun. The Sun is constantly emitting dangerous radiation and plasma which in some cases can affect or damage the systems on Earth. Scientists have an interest in studying this interaction and therefore visualizations of space weather data are useful. OpenSpace is an interactive software that visualizes the entire known universe with real-time data. OpenSpace supports a range of different visualization methods and techniques, for this work, the relevant visualization tools are field lines and cut planes. GAMERA is a simulation model that simulates a wide range of situations where plasma is subjected to the influence of magnetic fields, the simulations are based on curvilinear grids. This project focuses on implementing data from GAMERA into OpenSpace. OpenSpace already supports a variety of different simulation models, although none that uses curvilinear grids for the data. The curvilinear grid can adapt to the specific shape and geometry of the data, allowing for more accurate data representation. The project aims to create a pipeline for reading data files from simulation runs and visualize it as field lines and cut planes. The files used in this project contain data suitable for volumes and field lines. The method was to first develop a reader to extract and manage desired data from HDF5 files in which the simulation data is stored. The data used to visualize field lines is rendered with an already existing component in OpenSpace. Secondly, a slice operation was developed to extract cut planes from the files containing data for volume visualization, these are then visualized with the help of a component for rendering cut planes which was developed during this work. The work led to a pipeline that reads and manages simulation data from GAMERA and the data is successfully visualized. However, there is room for improvement in color rendering, robustness and level of user interaction during runtime. / <p>Examensarbetet är utfört vid Institutionen för teknik och naturvetenskap (ITN) vid Tekniska fakulteten, Linköpings universitet</p>