The Rosetta spacecraft orbited around comet 67P/Churyumov-Gerasimenko from 2014 to 2016. During this time, several thousands of cometary jets occurred and were photographed by the onboard cameras. Since the spacecraft slowly orbited around the comet nucleus and assuming an angular spread of 20º for the jets, it can be assumed that sometimes Rosetta flew through some of them. The dust particles ejected from the jet travel radially outward virtually unaffected by gravity, but as the jet is ongoing for several hours and as the comet nucleus rotates, the dust trace forms a spiral-like trajectory shape in space. Tracking the spacecraft's position around the times the jets were photographed, and checking whether it was within the dust cone, we found that Rosetta travelled across 181 out of the 3946 listed jets. Then, we looked into the plasma density and spacecraft potential data for every jet, finding some interesting events that could give rise to a further study into plasma interactions between jets and surrounding plasma in the cometary coma.

Earth-space traversing electromagnetic waves become attenuated as they propagate through the atmosphere. The sources of attenuation are weather phenomena in the Troposphere, and scintillation and absorption in the Ionosphere. On behalf of Arctic Space Technologies AB, an empirical model based on data from the last decade was built in Python, in order to estimate the level of attenuation and provide a better picture of the frequency environment at the site in Piteå. By utilizing recommendations from the International Telecommunication Union Radiocommunication Sector, and constraining the project to only consider the case where the satellite is at an 5° apparent elevation in Piteå, and a range of weather phenomena a nuanced picture can be obtained. It was found that the attenuation from the Ionosphere in typical satellite frequency bands is not of significance, and therefore only the Tropospheric sources were considered. The results showed that the S-band is the most reliable band to utilize, since little to no changes were observed for a range of weather scenarios. For the X-band, larger changes in the level of attenuation were observed for higher levels of precipitation, yet not as severe as for the Ku- and Ka- bands. However, for the Ku- and Ka-bands, large fluctuations in the attenuation were observed for different cases. In conclusion, the attenuation at Arctic space's site in Piteå for the S- and X-bands are the lowest and least effected by changes in weather. On the other hand, the Ku- and Ka-bands should be used predominantly under good weather circumstances.

High speed plasma flows (jets) are ubiquitous phenomena in the universe. For example, they carry energy from the most powerful sources (e.g active galactic nucleï AGN) to the medium at rest surrounding them. When the plasma at rest encounters the front of the fast flow, it gains energy via conversion from magnetic field energy to particle heating and acceleration. High speed plasma flows are also common in planetary magnetospheres including the Earth's magnetotail. In particular the fast Earthward magnetic reconnection outflows in the Earth's magnetotail provide a laboratory to address some of the open questions related to plasma jet fronts and the associated energy conversion. In this thesis, we use the four Magnetospheric Multiscale (MMS) spacecraft to investigate current sheet flapping, particle heating and particle acceleration associated with the fast magnetotail flows. In paper I, we investigate a short-period kink-like flapping motion of an ion scale current sheet in the wake of a plasma jet front. We show that the kink-like motion propagates along the current direction toward the flank of the magnetosphere, and that the prediction of the wavelength of the drift-kink instability of a thin current sheet agrees with our estimation of the wavelength of the observed kink-like current sheet. In paper II, we investigate particle acceleration at turbulent Earthward jet fronts during a moderately active substorm. We show that a proton with a gyroradius smaller than the scale of the Earthward convected structures gain energy from the bulk flow. On the other hand, we show that, depending on the time scale of the electromagnetic fluctuations with respect to the proton scale, protons with larger gyroradius get accelerated via resonant interaction with the jet front or via direct acceleration by the dawn-dusk electric field in a spatially limited electric field pulse.

Collisionless shocks are one of the most peculiar phenomena in space where non-linear collective phenomena in the plasma dominate the dynamics. They are believed to be one of the most efficient particle accelerators in the universe, and have internal dynamics that are yet to be fully explored. In this project we aim to understand the interplay between the electrostatic turbulence in the shock ramp and the electron dynamics leading to thermalization across the shock. To do so we first use a machine learning technique to compile a database of shocks crossings observed by magnetospheric multiscale (MMS), which will facilitate both case studies and statistical studies of shocks using MMS. The database contains 2803 shock crossings spanning a period from October 2015 to December 2020. For each crossing we provide key parameters necessary for understanding shock dynamics such as Alfv\'nic Mach number and the angle  between the upstream magnetic field and the vector normal to the shock $\theta_$. We then study whistler waves upstream of 11 quasiperpendicular supercritical shocks. We first apply four spacecraft timing method to magnetic field data from MMS to properly characterize the observed whistler waves. We determine their frequency in the plasma rest frame to range from 0.3 to 1.2 the lower hybrid frequency,their wavelength to range from 0.7 to 1.7 ion inertial length and $\theta_$ to range between $20^\circ$ and $42^\circ$. We then use particle data provided by MMS to show that a reflected beam component in the ion velocity distribution function is in resonance with the observed waves indicating that a kinetic cross field streaming instability (KCFSI) is behind the generation of such waves. Finally a kinetic solver is used to model to observed distribution and reinforce the previous conclusion that the KCFSI is behind the generation of the observed whistlers. We end this thesis by discussing the ongoing projects pertaining to the interaction of electrostatic wave mode determination in the shock ramp and the correlation between whistler waves and electrostatic waves around quasi-perpendicular shocks.

The results of past studies indicate that there is an influence of the presence of a nonzero dusk-dawn i.e. y component of the interplanetary magnetic field(IMF By) on the near-Earth magnetotail. Specifically, on the dusk-dawn component (By) of the magnetic field and plasma ion convection, resulting in interhemispheric asymmetries. This project aimed to investigate whether the same is true for mid-tail distances (around 60 RE downtail, at around the moon distance) by investigating data from the ARTEMIS P1 satellite and the OMNI IMF database. This was done by first filtering the data to only include plasma sheet data using criteria on ion temperature and density, and then constructing averages of both tail By and the ion velocity perpendicular to the magnetic field. These average were constructed separately for clearly positive IMF By (> 3 nT) and clearly negative IMF By (< -3 nT), and separately for the northern and southern plasma sheet. It was found that there is a clear effect of the sign of IMF By on both tail By and ion flows, leading to asymmetries similar to those reported at near-Earth distances. Thus it can be concluded that the presence of clearly nonzero IMF By affects the mid-tail region as well, and potentially the entire magnetotail. While these results are consistent with near-Earth studies, this is the first time the asymmetries due to nonzero IMF By are reported in the mid-tail.

Plasma physics emerged in the early 20th century and became a focal point for research after the Second World War due to the potential uses of nuclear fusion.The reasons for this varied from the creation of hydrogen bombs to fusion for energy production. Moreover, with recent developments in semiconductors and nanoscale objects, where quantum effects are non-negligible, a theory of quantum plasma wasrequired. Plasmas can be split into two main regimes, Classical and Quantum, each requiring a separate theory. In this thesis, we introduce the kinetic theory of plasmas. We study the two regimes separately and obtain a description of the plasmas in terms of a phase-space distribution function; a distribution 𝑓 in the classical case, and the quantum analogue in the Wigner function 𝑊. These are governed by the classical Vlasov equation and the quantum analogue in the Wigner equation. The introduction of the Wigner function in Wigner’s article [5] in 1932, made it easier to connect the two theories since theyboth reside within the phase space. To show that the quantum theory is equivalent to the classical theory with the addition of quantum effects, we used perturbation theory, with a perturbation in the form of an electrostatic linear wave. This results in two dispersion relations, one for each regime. These are equal except for a single term, which can be interpreted as quantum effects. This confirms that the two theories are equivalent in the classical limit. Moreover, we introduce the density matrix, a way to describe systems with statistical mixtures of quantum states. This enables us to derive the set of equations known as the BBGKY-hierarchy. In turn, this hierarchy allows us to reduce the number of particles we need to consider, something that comes in handy when dealing with many-particle systems, which otherwise can be close to impossible.

The Earth’s magnetosheath is a space plasma region consisting of solar wind plasma which is heated and compressed due to interaction with the Earth’s magnetic field. This turbulent region contains coherent structures and various plasma waves which affect the particle dynamics and collisionless energy transfer. In this licentiate thesis, we investigate such processes and where they occur. Through in-situ measurements from NASA’s Magnetospheric Multiscale (MMS) mission, we study whistler waves – electromagnetic, right-hand polarized waves known to heat electrons – and how they interact with electrons. We show how whistler waves are generated by electrons in the turbulent magnetosheath. We also investigate which plasma conditions are favorable for whistler waves to form.

We study plasma density variations within the ionosphere and their effects on trans-ionospheric signals, with a geodetic focus on Sweden from 2014 to 2023. We look for temporal, spatial, seasonal, and solar cycle patterns. We also discuss the percentage of occurrence of ionospheric irregularities and GNSS signal disturbances within the data at hand. We use in situ data collected by ESA-Swarm satellites and ground data provided by the Lantmäteriet-Swepos network ionosphere monitor. We find that high-latitude regions are susceptible to displaying more irregular electron density fluctuations (i.g., polar cap patches) than mid-latitudes. We also find that GNSS signal interference resulting in increased receivers’ positioning uncertainty is predominant at high latitudes. On the other hand, increased positioning uncertainty may be detected at noon in mid-latitude regions, mainly due to solar radiation exposure. Furthermore, hourly geomagnetic effects at high latitudes induce enhanced electron density fluctuations and positioning uncertainty at night. Findings also show more electron density fluctuations around winter and less in summer. Moreover, we find that the solar cycle influences the intensity of electron density fluctuations and positioning uncertainty, with the seasonal effects being more pronounced during periods of increased solar activity. Finally, results show that when ionospheric irregularities are observed, disturbances in GNSS signals may be detected, leading to imprecision in positioning services. Furthermore, we see that the absence of ionospheric irregularities results in a generally safe path for GNSS signals, which is beneficial for positioning accuracy. This comprehensive research enhances our understanding of ionospheric behavior in higher latitude environments and its impact on GNSS signals. Future research in this field could go deeper into the specific mechanisms driving electron density fluctuations and scintillation effects, explore additional geographic regions, and consider longer periods to refine our understanding of ionospheric dynamics and its implications for advanced space weather forecasting and satellite system resilience.

High-Power Microwaves (HPM) can be used to intentionally disturb or destroy electronic equipment at a distance by inducing high voltages and currents. This thesis presents results from experiments with a narrow band HPM source, the vircator. The high voltages needed to generate HPM puts the vircator under great stress, especially the electrode materials. Several electrode materials have been tested for endurance and their influence on the characteristics of the microwave pulse. With the proper materials the shot-to-shot variations are small and the geometry can be optimized in terms of e.g. output power or frequency content. Experiments with a resonant cavity added to the vircator geometry showed that with proper tuning of the cavity, the frequency content of the microwave radiation is very narrow banded and the highest radiated fields are registred. Since HPM pulses are very short and have high field strengths, special field probes are needed. An HPM pulse may shift in frequency during the pulse so it is very important to be able to compensate for the frequency dependence of the entire measurement system. The development and use of a far-field measurement system is described. / QC 20110616

In this work we have studied linear wave propagation in magnetized plasmas using a fully relativistic kinetic equation of spin-1/2 particles in the long scale approximation. The linearized kinetic equation is very long and complicated, hence we worked with restricted geometries in order to simplify the calculations. The dispersion relation of the relativistic model was calculated and compared with a dispersion relation from a previous work at the semi-relativistic limit. Moreover, a new mode was discovered that survives in the zero temperature limit. The origin of the mode in the kinetic equation was discussed and derived from a non-relativistic kinetic equation from a previous work.