Observations by spacecraft such as ACE, STEREO, and others show that there are proton spectral "breaks" with energy E-br at 1-10 MeV in some large CME-driven shocks. Generally, a single shock with the diffusive acceleration mechanism would not predict the "broken" energy spectrum. The present paper focuses on two converging shocks to identify this energy spectral feature. In this case, the converging shocks comprise one forward CME-driven shock on 2006 December 13 and another backward Earth bow shock. We simulate the detailed particle acceleration processes in the region of the converging shocks using the Monte Carlo method. As a result, we not only obtain an extended energy spectrum with an energy "tail" up to a few 10 MeV higher than that in previous single shock model, but also we find an energy spectral "break" occurring on similar to 5.5 MeV. The predicted energy spectral shape is consistent with observations from multiple spacecraft. The spectral "break," then, in this case is caused by the interaction between the CME shock and Earth's bow shock, and otherwise would not be present if Earth were not in the path of the CME.

We investigate the physics of charged-particle acceleration at spherical shocks moving into a uniform plasma containing a turbulent magnetic field with a uniform mean. This has applications to particle acceleration at astrophysical shocks, most notably, to supernovae blast waves. We numerically integrate the equations of motion of a large number of test protons moving under the influence of electric and magnetic fields determined from a kinematically defined plasma flow associated with a radially propagating blast wave. Distribution functions are determined from the positions and velocities of the protons. The unshocked plasma contains a magnetic field with a uniform mean and an irregular component having a Kolmogorov-like power spectrum. The field inside the blast wave is determined from Maxwell's equations. The angle between the average magnetic field and unit normal to the shock varies with position along its surface. It is quasi-perpendicular to the unit normal near the sphere's equator, and quasi-parallel to it near the poles. We find that the highest intensities of particles, accelerated by the shock, are at the poles of the blast wave. The particles "collect" at the poles as they approximately adhere to magnetic field lines that move poleward from their initial encounter with the shock at the equator, as the shock expands. The field lines at the poles have been connected to the shock the longest. We also find that the highest-energy protons are initially accelerated near the equator or near the quasi-perpendicular portion of the shock, where the acceleration is more rapid.

京都大学 / 新制・課程博士 / 博士(理学) / 甲第24405号 / 理博第4904号 / 新制||理||1700(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 鶴 剛, 教授 井岡 邦仁, 教授 永江 知文 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

Recent observations have shown that coronal shocks driven by coronal mass ejections can develop and accelerate particles within several solar radii in large solar energetic particle (SEP) events. Motivated by this, we present an SEP acceleration study that including the process in which a fast shock propagates through a streamer-like magnetic field with both closed and open field lines in the low corona region. The acceleration of protons is modeled by numerically solving the Parker transport equation with spatial diffusion both along and across the magnetic field. We show that particles can be sufficiently accelerated to up to several hundred MeV within 2-3 solar radii. When the shock propagates through a streamer-like magnetic field, particles are more efficiently accelerated compared to the case with a simple radial magnetic field, mainly due to perpendicular shock geometry and the natural trapping effect of closed magnetic fields. Our results suggest that the coronal magnetic field configuration is an important factor for producing large SEP events. We further show that the coronal magnetic field configuration strongly influences the distribution of energetic particles, leading to different locations of source regions along the shock front where most high-energy particles are concentrated. This work may have strong implications for SEP observations. The upcoming Parker Solar Probe will provide in situ observations for the distribution of energetic particles in the coronal shock region, and test the results of the study.

In this thesis, I use the new generation of radio interferometer along with X-ray observations to investigate the dynamics and energetics of radio-loud active galaxies which are key to understanding AGN feedback and the evolution of galaxies as a whole. I present new JVLA observations of powerful radio source and use innovative techniques to undertake a detailed analysis of JVLA observations of powerful radio galaxies. I compare two of the most widely used models of spectral ageing, the Kardashev-Pacholczyk and Jaffe-Perola models and also results of the more complex, but potentially more realistic, Tribble model. I find that the Tribble model provides both a good fit to observations as well as providing a physically realistic description of the source. I present the first high-resolution spectral maps of the sources and find that the best-fitting injection indices across all models take higher values than has previously been assumed. I present characteristic hot spot advance speeds and compare them to those derived from dynamical ages, confirming that the previously known discrepancy in speed remains present in older radio sources even when ages are determined at high spectral and spatial resolutions. I show that some previously common assumptions made in determining spectral ages with narrow-band radio telescopes may not always hold. I present results from a study of the powerful radio galaxy 3C223 at low frequencies with LOFAR to determine its spectrum on spatially small scales and tightly constrain the injection index, which I find to be consistent with the high values found at GHz frequencies. Applying this new knowledge of the low energy electron population, I perform synchrotron / inverse-Compton model fitting and find that the total energy content of the radio galaxy lobes increases by a factor greater than 2 compared to previous studies. Using this result to provide revised estimates of the internal pressure, I find the northern lobe to be in pressure balance with the external medium and the southern lobe to be overpressured. I go on to present the first large sample investigation of the properties of jets in Fanaroff and Riley type I radio galaxies (FR-I) at X-ray energies based on data from the Chandra archive. I explore relations between the properties of the jets and the properties of host galaxies in which they reside. I find previously unknown correlations to exist, relating photon index, volume emissivity, jet volume and luminosity, and find that the previously held assumption of a relationship between luminosities at radio and X-ray wavelengths is linear in nature when bona fide FR-I radio galaxies are considered. In addition, I attempt to constrain properties which may play a key role in determination of the diffuse emission process. I test a simple model in which large-scale magnetic field variations are primarily responsible for determining jet properties; however, we find that this model is inconsistent with our best estimates of the relative magnetic field strengths in my sample.

Afin de protéger leurs systèmes de détection de l'impulsion électromagnétique géante générée par l'interaction du laser PETAL avec sa cible, les diagnostics de PETAL seront équipés de détecteurs passifs. Pour les ensembles SEPAGE et SESAME, une combinaison d'Imaging Plates (IP) et de couches de protection de matériaux de grand numéro atomique sera utilisée, qui permettra: 1) d'assurer que la réponse des détecteurs sera indépendante de son environnement mécanique proche dans les diagnostics et donc homogène sur toute la détection, 2) de blinder les détecteurs contre les photons de haute énergie produits dans la cible de PETAL. Dans le travail présenté ici, nous avons réalisé des expériences d'étalonnage avec les IPs auprès d'installations générant des électrons, des protons ou des ions, dans le but de couvrir le domaine en énergie cinétique de la détection des particules chargées de PETAL, de 0.1 à 200 MeV. L'introduction a pour but de décrire les méthodes et outils utilisés au cours de cette étude. Le second chapitre présente les résultats de deux expériences réalisées avec des électrons dans le domaine d'énergie cinétique [5-180] MeV. Le troisième chapitre décrit une expérience et ses résultats avec les protons entre 80 et 200 MeV étaient envoyés sur nos détecteurs. Le quatrième chapitre est consacré à une expérience utilisant des protons et des ions entre1 et 22 MeV en énergie de protons et dont l'objectif était l'étude de détecteurs et le test du démonstrateur de SEPAGE. Nous avons utilisé GEANT4 pour l'analyse de nos données et prédire la réponse de nos détecteurs dans le domaine 0.1 à 1000 MeV. / In order to protect their detection against the giant electromagnetic pulse generated by the interaction of the PETAL laser with its target, PETAL diagnostics will be equipped with passive detectors. For SESAME and SEPAGE systems, a combination of imaging plate (IP) detectors with high-Z material protection layers will be used to provide additional features such as: 1) Ensuring a response of the detector to be independent of its environment and hence homogeneous over the surface of the diagnostics; 2) Shielding the detectors against high-energy photons from the PETAL target. In this work, calibration experiments of such detectors based on IPs were performed at electron and proton facilities with the goal of covering the energy range of the particle detection at PETAL from 0.1 to 200 MeV. The introduction aims at providing the reader the methods and tools used for this study. The second chapter presents the results of two experiments performed with electrons in the range from 5 to 180 MeV. The third chapter describes an experiment and its results, where protons in the energy range between 80 and 200 MeV were sent onto detectors. The fourth chapter is dedicated to an experiment with protons and ions in the energy range from 1 to 22 MeV proton energy, which aimed at studying our detector responses and testing the demonstrator of the SEPAGE diagnostic. We used the GEANT4 toolkit to analyse our data and compute the detection responses on the whole energy range from 0.1 to 1000 MeV.

La microscopie électronique et la diffraction d’électrons ont permis de comprendre l’organisation des atomes au sein de la matière. En utilisant une source courte temporellement, il devient possible de mesurer les déplacements atomiques ou les modifications de la distribution électronique dans des matériaux. A ce jour, les sources ultra-brèves pour les expériences de diffraction d’électrons ne permettent pas d’atteindre une résolution temporelle inférieure à la centaine de femtosecondes (fs). Les accélérateurs laser-plasma sont de bons candidats pour atteindre une résolution temporelle de l’ordre de la femtoseconde. De plus, ces accélérateurs peuvent fonctionner à haut taux de répétition, permettant d’accumuler un grand nombre de données.Dans cette thèse, un accélérateur laser-plasma fonctionnant au kHz a été développé et construit. Cette source accélère des électrons à une énergie de 100 keV environ à partir d’impulsions laser d’énergie 3 mJ et de durée 25 fs. La physique de l’accélération a été étudiée, démontrant entre autres l’effet du front d’onde laser sur la distribution transverse des électrons.Les premières expériences de diffraction avec ce type de sources ont été réalisées. Une expérience de preuve de principe a montré que la qualité de la source est suffisante pour obtenir de belles images de diffraction sur des feuilles d’or et de silicium. Dans un second temps, la dynamique structurelle d’un échantillon de Silicium a été étudiée avec une résolution temporelle de quelques picosecondes, démontrant le potentiel de ce type de sources.Pour augmenter la résolution temporelle à sub-10 fs, il est nécessaire d’accélérer les électrons à des énergies relativistes de quelques MeV. Une étude numérique a montré que l’on peut accélérer des paquets d’électrons ultra-courts grâce à des impulsions laser de 5 mJ et 5 fs. Il serait alors possible d’atteindre une résolution temporelle de l’ordre de la femtoseconde. Finalement, une expérience de post-compression des impulsions laser due à l’ionisation d’un gaz a été réalisée. La durée du laser a pu être réduite d’un facteur deux, et l’homogénéité de ce processus a été étudiée expérimentalement et numériquement. / Electronic microscopy and electron diffraction allowed the understanding of the organization of atoms in matter. Using a temporally short source, one can measure atomic displacements or modifications of the electronic distribution in matter. To date, the best temporal resolution for time resolved diffraction experiments is of the order of a hundred femtoseconds (fs). Laser-plasma accelerators are good candidates to reach the femtosecond temporal resolution in electron diffraction experiments. Moreover, these accelerators can operate at a high repetition rate, allowing the accumulation of a large amount of data.In this thesis, a laser-plasma accelerator operating at the kHz repetition rate was developed and built. This source generate electron bunches at 100 keV from 3 mJ and 25 fs laser pulses. The physics of the acceleration has been studied, and the effect of the laser wavefront on the electron transverse distribution has been demonstrated.The first electron diffraction experiments with such a source have been realized. An experiment, which was a proof of concept, showed that the quality of the source permits to record nice diffraction patterns on gold and silicium foils. In a second experiment, the structural dynamics of a silicium sample has been studied with a temporal resolution of the order of a few picoseconds.The electron bunches must be accelerated to relativistic energies, at a few MeV, to reach a sub-10 fs temporal resolution. A numerical study showed that ultra-short electron bunches can be accelerated using 5 fs and 5 mJ laser pulses. A temporal resolution of the order of the femtosecond could be reached using such bunches for electron diffraction experiments. Finally, an experiment of the ionization-induced compression of the laser pulses has been realized. The pulse duration was shorten by a factor of 2, and the homogeneity of the process has been studied experimentally and numerically.