Magnetic reconnection is a universal process occurring at boundaries between magnetized plasmas, where changes in the topology of the magnetic field lead to the transport of charged particles across the boundaries and to the conversion of electromagnetic energy into kinetic and thermal energy of the particles. Reconnection occurs in laboratory plasmas, in solar system plasmas and it is considered to play a key role in many other space environments such as magnetized stars and accretion disks around stars and planets under formation. Magnetic reconnection is a multi-scale plasma process where the small spatial and temporal scales are strongly coupled to the large scales. Reconnection is initiated rapidly in small regions by microphysical processes but it affects very large volumes of space for long times. The best laboratory to experimentally study magnetic reconnection at different scales is the near-Earth space, the so-called Geospace, where Cluster spacecraft in situ measurements are available. The European Space Agency Cluster mission is composed of four-spacecraft flying in a formation and this allows, for the first time, simultaneous four-point measurements at different scales, thanks to the changeable spacecraft separation. In this thesis Cluster observations of magnetic reconnection in Geospace are presented both at large and at small scales. At large temporal (a few hours) and spatial (several thousands km) scales, both fluid and kinetic evidence of reconnection is provided. The evidence consist of ions accelerated and transmitted across the Earth’s magnetopause. The observations show that component reconnection occurs at the magnetopause and that reconnection is continuous in time. The microphysics of reconnection is investigated at smaller temporal (a few ion gyroperiods) and spatial (a few ion gyroradii) scales. Two regions are important for the microphysics: the X-region, around the X-line, where reconnection is initiated and the separatrix region, away from the X-line, where most of the energy conversion occurs. Observations of a separatrix region at the magnetopause are shown and the microphysics is described in detail. The separatrix region is shown to be highly structured and dynamic even away from the X-line. Finally the discovery of magnetic reconnection in turbulent plasma is presented by showing, for the first time, in situ evidence of reconnection in a thin current sheet found in the turbulent plasma downstream of the quasi-parallel Earth’s bow shock. It is shown that turbulent reconnection is fast and that electromagnetic energy is converted into heating and acceleration of particles in turbulent plasma. It is also shown that reconnecting current sheets are abundant in turbulent plasma and that reconnection can be an efficient energy dissipation mechanism.

Nesta tese é analisada a dinâmica de uma partícula relativística se movendo sob a influência de um campo magnético uniforme e uma onda eletrostática e estacionária dada na forma de pulsos periódicos. O mapa que descreve a evolução temporal do sistema é explícito e pode ser considerado como uma versão relativística e magnetizada do mapa padrão clássico. A posição aproximada dos pontos periódicos é calculada analiticamente e com essa informação é possível estudar as ressonâncias primárias. Para o sistema em estudo, observa-se que a maior parte das ressonâncias possui mais de uma cadeia de ilhas. Isso ocorre pois o sistema apresenta um número infinito de termos ressonantes com o mesmo número de rotação e que podem gerar ilhas na mesma posição do espaço de fases. Verifica-se que essa superposição de termos ressonantes faz com que o número de cadeias varie em função dos parâmetros da onda. Para valores de período ou número de onda suficientemente elevados, todas as ressonâncias primárias apresentam duas ou mais cadeias de ilhas no espaço de fases. As ilhas de ressonância primária são utilizadas nesta tese para acelerar partículas de forma regular. Em particular, considera-se a ressonância principal do sistema, para a qual a energia inicial da partícula pode estar muito próxima de sua energia de repouso se os parâmetros da onda forem adequados. Além disso, aplica-se um método de controle do caos para Hamiltonianas quase integráveis que consiste na adição de um termo de controle simples e com baixa amplitude ao sistema. Esse termo de controle cria toros invariantes em todo o espaço de fases que confinam as trajetórias caóticas em pequenas regiões, tornando a dinâmica controlada mais regular. Verifica-se numericamente que o termo de controle reduz drasticamente as regiões caóticas. Além disso, observa-se que o controle do caos e a consequente recuperação de trajetórias periódicas e quase periódicas no espaço de fases podem ser utilizados para melhorar o processo de aceleração regular de partículas. / In this thesis, we analyze the dynamics of a relativistic particle moving under the influence of a uniform magnetic field and a stationary electrostatic wave given as a series of periodic pulses. The map that describes the time evolution of the system is explicit, and it can be considered as a magnetized relativistic version of the classical standard map. We calculate analytically the approximate position of the periodic points and we use this information to study the primary resonances. For the system under study, we observe that most of its resonances exhibit more than one island chain. It occurs because the system presents an infinite number of resonant terms with the same winding number that may generate islands in the same position of phase space. We verify that this superposition of resonant terms makes the number of chains vary as a function of the parameters of the wave. For sufficiently large values of the wave period or wave number, all the primary resonances present two or more island chains in phase space. We use the islands of primary resonances in this thesis to regularly accelerate particles. In particular, we consider the main resonance of the system, for which the initial energy of the particle can be very close to its rest energy if the parameters of the wave are adequate. Furthermore, we apply a method of control of chaos for near-integrable Hamiltonians that consists in the addition of a simple control term with low amplitude to the system. This control term creates invariant tori in the whole phase space that confine the chaotic trajectories to small regions, making the controlled dynamics more regular. We verify numerically that the control term drastically reduces the chaotic regions. Moreover, we observe that the control of chaos and the consequent recovery of periodic and quasiperiodic trajectories in phase space can be used to improve the process of regular particle acceleration.

The thesis at hand addresses design, characterization and experimental testing of pulsed high-field magnets for utilization in the field of laser-plasma physics. The central task was to establish a technology platform that allows to manipulate laser-driven ion sources in a way that the accelerated ions can be used in complex application studies, e.g. radiobiological cell or tumor irradiation. Laser-driven ion acceleration in the regime of target normal sheath acceleration (TNSA) offers the unique opportunity to accelerate particles to kinetic energies of few 10MeV on the micrometer scale. The generated bunches are short, intense, show broad exponentially decaying energy spectra and high divergence. In order to efficiently use the generated particles, it is crucial to gain control over their divergence directly after their production. For most applications it additionally is favorable to reduce the energy spread of the beam. This work shows that the developed pulsed high-field magnets, so-called solenoids (cylindrical magnets), can efficiently capture, transport and focus laser-accelerated protons. The chromaticity of the magnetic lens thereby provides for energy selection. Three prototype solenoids, adapted to fit different application scenarios, and associated current pulse drivers have been developed. The magnets generate fields of several 10 T. Pulse durations are of the order of one millisecond and thus the fields can be considered as quasi-static for laser-plasma interaction processes taking place on the ps- to ns-scale. Their high field strength in combination with abandoning magnetic cores make the solenoids compact and light-weight. The presented experiments focus on a solenoid magnet designed for the capture of divergent laser-driven ion beams. They have been carried out at the 6MV tandetron accelerator and the laser acceleration source Draco of Helmholtz-Zentrum Dresden – Rossendorf as well as at the PHELIX laser of GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt.

The origin of Ultra-High-Energy Cosmic Rays (UHECRs) is still an open question in Astrophysics. The scope of this thesis is the study of the termination shocks in the jets of radiogalaxies 3C 105, 3C 227, and 3C 445 as cosmic rays accelerators. We assume the diffusive shock acceleration (DSA) and that the maximum energy is determined by the escape of cosmic rays downstream of the shock due to the magnetization. We find maximum achievable energy of non-thermal electrons and protons, which appeared to be only~TeV. Therefore the reverse shocks of AGNs' jets are not the sources of UHECRs. We also implement the model, where the scattering centers for the DSA emerge from the non- resonant hybrid instabilities in plasma. We take into account the results from the numerical simulations and observations that indicate the amplification of the magnetic field by orders of magnitude, and we obtain results that qualitatively fit the simulation outcome.

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No description available.

Durch die Fokussierung eines ultrakurzen und hochintensiven Laserpulses auf ein Festkörpertarget können Pulse von Protonen und anderen positiv geladenen Ionen mit Teilchenenergien von einigen MeV pro Nukleon erzeugt werden. Die Charakterisierung dieser Teilchenstrahlung erfordert die Identifizierung der Ionenspezies und die Bestimmung ihrer spektralen Verteilung möglichst nach jedem Puls. Im Rahmen dieser Diplomarbeit wurden zwei Spektrometer entwickelt und am DRACO-Lasersystem des Forschungszentrums Dresden implementiert. Neben der Inbetriebnahme eines Thomson-Spektrometers mit einer Mikrokanalplatte und einem Fluoreszenzschirm als Auslese erfolgte die Entwicklung eines Flugzeitspektrometers. Die Verwendung einer Mikrokanalplatte mit nur 180ps Anstiegszeit als Signalverstärker sorgt darin für eine verbesserte Energieauflösung und einen flexibleren Einsatz im Experimentierbetrieb. Ein dem Flugzeitsignal überlagertes Störsignal, welches durch die Einstreuungen eines elektromagnetischen Impulses in den Aufbau verursacht wurde, konnte erfolgreich durch die Anwendung verschiedener Filter unterdrückt werden. Als Ergebnis dieser Arbeit steht eine anwendungsbereite Diagnostik für laserbeschleunigte Protonen und Ionen zur Verfügung. / By focusing an ultra-short high-intensity laser pulse on a solid target, pulses of protons and other positive charged ions with energies of several MeV per nucleon are generated. It is necessary to identify the species of those particles and obtain their energy spectra in a single-shot regime. Within this diploma thesis two spectrometers have been developed and implemented in the DRACO-laboratory of the Forschungszentrum Dresden. Besides a Thomson spectrometer with read-out via microchannel plate and phosphor screen, a time-of-flight spectrometer was developed. The usage of a microchannel plate with 180ps rise time as a signal amplifier leads therein to a better energy resolution and a more flexible handling in experimental operation. A noise signal generated by stray pick-up of an electromagnetic pulse and superimposing the time-of-flight signal was considerably reduced by the application of different filters. As a result of this work a ready-to-use diagnostic for laser accelerated protons and ions is available.

Les propulseurs électriques sont de plus en plus utilisés pour des missions de correction de trajectoire des satellites et pourront dans un avenir proche être utilisés pour le transfert d’orbite. Ces propulseurs constituent une excellente alternative aux propulseurs chimiques grâce à leur rendement élevé et une substantielle économie de carburant réalisée par rapport aux propulseurs chimiques. Les propulseurs à effet Hall créent la poussée par l’accélération d’ions positifs de xénon ou de krypton dans un plasma confiné par un champ magnétique. L’objet de ce manuscrit concerne principalement les caractéristiques de l’accélération des ions et des atomes dans un propulseur à effet Hall. Les influences de la largeur du canal de décharge, de la topologie magnétique et de la cathode sur l’efficacité d’accélération des ions sont étudiées. Des pistes d’optimisation de l’architecture du propulseur sont alors proposées qui pourraient être particulièrement avantageuses sur les propulseurs de petite taille, comme l’élargissement du canal et l’augmentation du champ magnétique près des parois du canal. L’influence de la position et du potentiel de la cathode sur la déviation du faisceau ionique est révélée. L’évolution temporelle basse fréquence du champ électrique est mesurée par comptage synchrone de photons et suggère que la température atomique joue un rôle important dans les oscillations basse fréquence de la décharge. Par ailleurs, l’influence du champ magnétique sur les performances d’un propulseur proche des modèles de vol a été mesurée grâce à l’utilisation d’un moteur doté d’une topologie magnétique flexible. Ceci a montré la difficulté de définir un paramètre numérique capable de synthétiser l’information complexe de la répartition spatiale du champ magnétique dans le canal de décharge. Les très faibles modifications des performances par le champ magnétique soulignent l’importance de la précision dans la mesure. / Electric propulsion systems are more and more often used for trajectory correction of satellites and may soon be used for orbit transfer. These devices represent a great alternative to classic chemical propulsion devices thanks to their high efficiency and propellant mass savings. Hall effect thruster provide thrust by the acceleration of xenon or krypton ions in a magnetized confined plasma. The study presented in this manuscript mainly addresses characteristics of ion and atom acceleration in a Hall effect thruster. Influence of channel width, magnetic topology and cathode parameters on ion acceleration efficiency is investigated. Ways to optimize thruster architecture are suggested that may be particularly relevant for low power thrusters, such as widening thruster channel and increasing magnetic field amplitude near channel walls. Influence of cathode position with respect to the thruster channel exit plane and its potential with respect to ground on ion beam deviation has been revealed with two thrusters. Low frequency time evolution of the accelerating electric field was measured using lock-in photon counting system. Results strongly suggest that the atom temperature plays a crucial role in low frequency time evolution of the whole plasma discharge. Measurement of performances as a function of the magnetic field demonstrated that numeric parameters are compulsory to carry on a relevant parametric study. These parameters would summarize the 2D information of magnetic topology. Weak influence of magnetic topology revealed that thrust measurement precision needs to be increased by at least one order of magnitude if one wants to reach a better understanding of plasma confinement in a Hall effect thruster.

Après plus d'un siècle d'étude des rayons cosmiques, des questions persistent à propos de leur origine. À l'échelle de notre galaxie, les vestiges de supernovæ sont d'excellents candidats en tant que sources de rayons cosmiques et il est aujourd'hui avéré que ces ondes de choc générées par l'explosion d'étoiles en fin de vie accélèrent des électrons jusqu'au TeV. Cependant, des preuves tangibles manquent toujours pour confirmer que les protons, qui représentent ~90% du rayonnement cosmique, y sont également accélérés. Ces preuves sont à chercher entre 100 MeV et 10 GeV où la forme spectrale de l'émission gamma nous renseigne sur la nature des particules accélérées.Ce domaine en énergie est observé par le satellite Fermi qui scrute le ciel à haute énergie grâce au Large Area Telescope (LAT), un instrument capable de détecter les rayons gamma d'énergies comprises entre 20 MeV et plus de 300 GeV. Avec la dernière version des données en date (Pass 8) rendue publique en 2015, la surface efficace a été sensiblement accrue, notamment à haute énergie. L'objet de cette thèse a été de mettre à profit les nouvelles performances du LAT pour étudier le rayonnement provenant de jeunes vestiges de supernovæ en coquille afin d'évaluer leur capacité à accélérer des particules à haute énergie. Au total, quatre vestiges de ce type ont été étudiés en détail : RCW 86, HESS J1731-347, SN 1006 et RX J1713.7-3946.L'analyse morphologique et spatiale de ces sources nous a menés à d'importants résultats : HESS J1731-347 et SN 1006 ont été détectés pour la première fois au GeV, nous avons mis en évidence une morphologie en coquille pour RCW 86 qui était précédemment détectée comme une source ponctuelle et RX J1713.7-3946 a révélé une forme spectrale plus complexe que ce qui était alors connu. Grâce à la modélisation de l'émission non-thermique de ces sources, en s'aidant des données au TeV obtenues par H.E.S.S., nous avons montré que leur émission gamma est très largement dominée par le rayonnement Compton inverse des électrons de haute énergie diffusant sur les champs de photons ambiants. Cependant, des modifications spectrales ont également été trouvées dans certaines parties de SN 1006 et RX J1713.7-3946 où l'onde de choc est en interaction avec des régions denses en matière, traçant la possible accélération de protons en leur sein. / After more than a century of cosmic-ray studies, questions about their origin remain unanswered. In our galaxy, supernova remnants are excellent candidates to be the sources of cosmic rays and it is now certain that these shock waves created by the explosion of dying stars accelerate electrons up to TeV energies. However, undeniable proof is still missing to confirm that protons, which represent ~90% of the cosmic radiation, are also accelerated. Such proof can be searched for between 100 MeV and 10 GeV, where the spectral shape of the gamma-ray emission changes according to the nature of the particles that are accelerated.This energy range is covered by the Fermi spacecraft which observes the high energy sky with the Large Area telescope (LAT), an instrument detecting gamma-rays from 20 MeV to more than 300 GeV. With the latest version of the data, released in 2015 (Pass 8), the effective area has been greatly improved, especially at high energy. The goal of this thesis was to take advantage of the improved performance of the LAT to study the radiation coming from young shell-type supernova remnants and to evaluate their ability to accelerate particles to high energy. Four such remnants were studied in detail: RCW 86, HESS J1731-347, SN 1006 and RX J1713.7-3946.Spatial and spectral analyses of these sources yielded important results: HESS J1731-347 and SN 1006 were identified for the first time in the GeV range, we detected a shell-like morphology for RCW 86 which was previously seen as a point source, and RX J1713.7-3946 revealed an unexpected spectral shape. Broadband modeling of the non-thermal emission of these remnants, using in particular TeV data obtained with H.E.S.S., showed that their gamma-ray emission is dominated by the inverse Compton scattering of electrons on ambient photon fields. However, we also found spectral modifications in some parts of SN 1006 and RX J1713.7-3946 where the shock is interacting with dense regions that could trace the acceleration of protons.

Durch die Fokussierung eines ultrakurzen und hochintensiven Laserpulses auf ein Festkörpertarget können Pulse von Protonen und anderen positiv geladenen Ionen mit Teilchenenergien von einigen MeV pro Nukleon erzeugt werden. Die Charakterisierung dieser Teilchenstrahlung erfordert die Identifizierung der Ionenspezies und die Bestimmung ihrer spektralen Verteilung möglichst nach jedem Puls. Im Rahmen dieser Diplomarbeit wurden zwei Spektrometer entwickelt und am DRACO-Lasersystem des Forschungszentrums Dresden implementiert. Neben der Inbetriebnahme eines Thomson-Spektrometers mit einer Mikrokanalplatte und einem Fluoreszenzschirm als Auslese erfolgte die Entwicklung eines Flugzeitspektrometers. Die Verwendung einer Mikrokanalplatte mit nur 180ps Anstiegszeit als Signalverstärker sorgt darin für eine verbesserte Energieauflösung und einen flexibleren Einsatz im Experimentierbetrieb. Ein dem Flugzeitsignal überlagertes Störsignal, welches durch die Einstreuungen eines elektromagnetischen Impulses in den Aufbau verursacht wurde, konnte erfolgreich durch die Anwendung verschiedener Filter unterdrückt werden. Als Ergebnis dieser Arbeit steht eine anwendungsbereite Diagnostik für laserbeschleunigte Protonen und Ionen zur Verfügung. / By focusing an ultra-short high-intensity laser pulse on a solid target, pulses of protons and other positive charged ions with energies of several MeV per nucleon are generated. It is necessary to identify the species of those particles and obtain their energy spectra in a single-shot regime. Within this diploma thesis two spectrometers have been developed and implemented in the DRACO-laboratory of the Forschungszentrum Dresden. Besides a Thomson spectrometer with read-out via microchannel plate and phosphor screen, a time-of-flight spectrometer was developed. The usage of a microchannel plate with 180ps rise time as a signal amplifier leads therein to a better energy resolution and a more flexible handling in experimental operation. A noise signal generated by stray pick-up of an electromagnetic pulse and superimposing the time-of-flight signal was considerably reduced by the application of different filters. As a result of this work a ready-to-use diagnostic for laser accelerated protons and ions is available.