The most compelling evidence of the complex interaction between the geomagnetic field of the Earth and the magnetic field of the Sun is found in the polar ionosphere. Large scale F-region plasma density perturbations result from the coupling between the two fields. Plasma density enhancements known as ionization patches, and depletions can have lifetimes of several hours in the F region and are almost always present everywhere throughout the nighttime polar ionosphere. The perturbations can seed ionospheric irregularities that severely hamper communication and navigational networks, even during times of subdued geomagnetic activity. Up until recently, it has been difficult to study the perturbations due to the remoteness of their location. In the past decade an array of optical and radio instruments have been deployed to the Canadian sector of the Arctic, enabling a more thorough sampling of the polar ionosphere and the large scale perturbations therein. In this work, common volume measurements from the Rankin Inlet Super Dual Auroral Radar Network (SuperDARN), Resolute Bay Incoherent Scatter Radar - North (RISR-N) and Optical Mesosphere and Thermosphere Imagers (OMTI) system at Resolute Bay are employed to investigate the generation mechanisms, transport properties, and optical and radio signatures of the large scale perturbations. A model connecting the optical signatures of patches to their velocity profile through the ionosphere is introduced and applied to OMTI data. In addition, an algorithm is developed to detect the presence of patches using RISR-N. Using the algorithm, a survey of patches sampled over several days is conducted, providing a comprehensive account of the variable polar ionosphere in terms of its plasma state parameters. Furthermore, the algorithm is used to diagnose patches as a primary source of coherent backscatter for the Rankin Inlet SuperDARN radar. Lastly, the generation of a deep plasma density depletion is analyzed using the three aforementioned instruments. Using a model, it is shown that such perturbations can be forged by intense frictional heating events in the polar ionosphere on a time scale of 15 minutes, and can subsequently be transported through the region.

The high-latitude electric eld fall-o region connects convection in the polar cap to the region where ring currents modify the penetration electric field equatorward of the polar cap boundary. This region is often overlooked because it falls between the limits of low latitude and high-latitude ionospheric models. However, penetrating electric fields cause large changes in ion composition; and therefore, correctly modeling the electric fields and plasma drift in this region aids in correctly specifying the ionosphere. Many ionospheric models use the Kp index as a physical driver, and so the latitude dependence of the plasma drift in the fall-o region was investigated as a function of Kp using Defense Meteorological Satellite Program ion drift data from the 2007{2010 solar minimum. Both the dusk and dawn sectors were analyzed and t to analytical functions describing the fall-o with decreasing latitude. The latitude dependencies were found to dier in the dusk and dawn sectors with a factor of two increase in the expansion of the duskside polar cap radius and auroral region over the dawnside. Additionally, the low-Kp polar cap radius was found to be five degrees smaller than the radius currently used in simple ionospheric models.

Accurate knowledge of the electron density structure of the Earth's upper atmosphere is crucial to forecasting the performance of transionospheric radio signals. For this research, we focus on storm-time structuring in the mid- to high latitude ionosphere where large gradients in electron density can cause severe degradation of communication and navigation signals. We begin in Chapter 2 with a review of the primary data sets and methods used to accomplish the collaborative, multi-instrument studies described in this dissertation. In Chapter 3, we compare observational techniques for tracking polar cap patches during a moderate geomagnetic storm interval. For the first time, we monitor the transportation of patches with high spatial and temporal resolution across the polar cap for 1--2~h using a combination of GPS TEC, all-sky airglow imagers (ASIs), and Super Dual Auroral Radar Network (SuperDARN) HF radar backscatter. Simultaneous measurements from these data sets allow for continuous tracking of patch location, horizontal extent, and velocity even under adverse observational conditions for one or more of the techniques. A focus is placed on the structuring of patches, particularly on the nightside ionosphere as they become wider in the dawn-dusk direction and develop narrow finger-like structures. In Chapter 4, we perform a superposed epoch analysis to characterize the average response of GPS TEC in the North American sector during more than 100 geomagnetic storms over a 13-year interval. For the first time a rigorous approach is used to fully separate storm-time, local time, longitudinal, and seasonal effects at midlatitudes where dense ground receiver coverage is available. The rapid onset of a positive phase is observed across much of the dayside and evening ionosphere followed by a longer-lasting negative phase across all latitudes and local times. Our results show clear seasonal variations in the storm-time TEC, such that summer events tend to be dominated by the negative storm response while winter events exhibit a stronger initial positive phase with minimal negative storm effects. A prominent magnetic declination effect is identified and examined in terms of thermospheric zonal winds pushing plasma upward/downward along magnetic field lines of opposite declination. Finally in Chapter 5 we summarize several co-authored studies which examined various storm-time phenomena utilizing GPS TEC mapping tools developed for this dissertation research, with topics including subauroral polarization stream (SAPS), storm enhanced density (SED), tongue of ionization (TOI), and polar cap patches. / Ph. D.

Pc3-4 waves are recorded as geomagnetic pulsations with periods of 6-100s. They are generated at the bowshock and propagate to mid and auroral latitudes as Alfvén waves along closed magnetic field lines. At these latitudes Pc3-4 waves have been studied on the ground using magnetometers and in the ionosphere using HF radar. These waves have also been observed using magnetometers at polar latitudes even though there is no known propagation mechanism to the “open” field lines of the polar cap regions. In this work we used PolarDARN stations at Rankin Inlet and Inuvik to attempt the first study of Pc3-4 waves in the polar cap regions using radar. In ground scatter data, Doppler velocity oscillations with frequencies in the Pc3-4 range were found to be a common daytime occurrence. The oscillations are spatially coherent and in phase along the beam’s line of sight, matching lower latitude observations. However, upon further study it became apparent that the characteristics of the oscillations are different from those known for Pc3-4 waves. The observed oscillations have a diurnal trend that shows peaks in activity at 7:00 and 14:00MLT, where Pc3-4 oscillations have a diurnal peak at 10:30-11:00 MLT. In addition, poor coherence was observed between oscillations in radar and ground magnetic field variations at the nearby Taloyoak magnetometer. Further confounding the problem, we found that although the oscillations were coherent along the line-of-sight of the radar, poor coherence is observed when comparing oscillations in different beams separated by similar spatial scales. This finding counters both the spatial coherence observed along the beam’s line of sight and the spatial coherence of Pc3-4 waves at auroral latitudes. We conclude that it is unlikely that the observed oscillations are the result of Pc3-4 ULF waves. We instead propose that the observed Doppler velocity oscillations are caused by a change in the ionization along the ray’s path due to auroral particle precipitation.

Atmospheric mass is transported in and out of the stratospheric polar cap region by a wave-driven meridional circulation. Using composites of polar cap pressure anomalies, defined as deviations from the average annual cycle, it is shown that this stratospheric mass flux is accompanied by a similar mass flux near the surface. This 'tropospheric amplification' of the stratospheric signal is introduced as a new way to quantify stratosphere-troposphere coupling. Regression analysis is used to create a vertical profile of atmospheric pressure during a tropospheric amplification event, and the regression slope profile is used as a tool to quantify the amplification. Using data from 5 reanalysis datasets and 11 climate models, it is shown that high-top models, with a model lid of above 1 hPa, are significantly better at reproducing tropospheric amplification than low-top models, due to having more detailed parameterisations of stratospheric processes. However, the regression slope profiles of all models, bar one, are significantly different to the profile of reanalysis data at a 95% confidence level. Tropospheric amplification is also investigated in historical and future simulations from these models, and it is concluded that there is not expected to be a large change in the phenomenon over the next 100 years. The processes needed to reproduce tropospheric amplification can be identified by comparing idealised models of different complexity. A simple dry-core model is not able to reproduce tropospheric amplification, while a model with a comprehensive radiation scheme does produce the basic regression slope profile under certain configurations. The associations between pressure change and mass flux are further investigated using primitive equations. It is found that vertical and horizontal contributions to mass flux act to mostly cancel each other out, leaving a poorly-conditioned residual, and that the horizontal mass flux across the polar cap boundary has both geostrophic and ageostrophic components.

Measurements with satellite and sounding rocket borne instruments contain important information on remote and local processes in regions containing matter in the plasma state. The characteristic features of the particle distributions can be used to explain the morphology and dynamics of the different plasma populations. Charged particles are lost from a region due to precipitation into the atmosphere, charge exchange processes, or convection to open magnetic field lines. The sources of the Earth’s magnetospheric plasma are mainly ionization and extraction of upper atmosphere constituents, and entry of solar wind plasma. The intensity and distribution of auroral precipitation is controlled in part by the conditions of the interplanetary magnetic field causing different levels of auroral activity. Acceleration of electrons and positive ions along auroral field lines play an important role in magnetospheric physics. Electric fields that are quasi-steady during particle transit times, as well as fluctuating fields, are important for our understanding of the behaviour of the plasma in the auroral region. High-resolution data from the Swedish Viking and the Swedish/German Freja satellites have increased our knowledge considerably about the interaction processes between different particle populations and between particles and wave fields. This thesis describes acceleration processes influencing both ions and electrons and is based on in-situ measurements in the auroral acceleration/heating region, with special emphasis on; processes at very high latitudes, the role of fluctuating electric fields in producing so called electron conics, and positive ion heating transverse to the geomagnetic field lines. / <p>Diss. (sammanfattning) Umeå : Umeå universitet, 1994, härtill 6 uppsatser.</p> / digitalisering@umu.se

Ionospheric effects are one of the factors that can have negative impact on Global Navigation Satellite Systems (GNSS). Those effects can be called medium-scale traveling ionospheric disturbances (MS-TIDs) at middle latitude regions and polar cap patches at high latitude regions. The ionospheric variations have different patterns for each region and time. The statistical measures of the ionospheric variation are analyzed presented as functions of time in half solar cycle, annual seasonal, and time of day for four geographical locations in Sweden. By processing achieved GPS data from a 7-year period, 2013-2020, from SWEPOS, the characterization of the ionospheric variation was performed. It is found that the ionospheric variation is larger for the Norra Norrland region during solar minimum. However, during solar maximum, the variation depends on the seasons but high variation seems to occur the most in Svealand region. For the more northern regions (Norra and Södra Norrland), the ionospheric variation is greater during nighttime than during daytime, while for the more southern regions (Svealand and Götaland), the variation is greater during daytime. At solar maximum, the variability is higher during the months March, May, September, and October and smaller in June, July, and August. For the ionospheric variation prediction, a model based on Recurrent Neural Network (RNN) called Long Short-Term Memory (LSTM) is proposed. The tuned hyperparameters for LSTM are tested for the prediction accuracy by comparing the predicted values to the measured values. It is found that the LSTM can yield the prediction results with more than 90% accuracy when using 1-6 hours of input data and aiming for 10-35 minutes of output data. Longer duration of input and output results in lower accuracy of the predicted values. / Jonosfäriska effekter är en av de faktorer som kan ha negativ inverkan på Global Navigation Satellite Systems (GNSS). Dessa effekter kan kallas medelstora resande jonosfäriska störningar (MS-TID) vid mellanliggande latitudområden och polarkapslar på områden med hög latitud. De jonosfäriska variationerna har olika mönster för varje region och tid. De statistiska måtten på den jonosfäriska variationen analyseras presenterade som tidsfunktioner i halva solcykeln, årssäsong och tid på dygnet för fyra geografiska platser i Sverige. Genom att bearbeta uppnådda GPS-data från en 7-årsperiod, 2013-2020, från SWEPOS, utfördes karaktäriseringen av den jonoshperiska variationen. Det har visat sig att den jonosfäriska variationen är större för Norra Norrland -regionen under solminimum. Under solens maximala beror variationen dock på årstiderna men hög variation tycks förekomma mest i Svealandsregionen. För de mer norra regionerna (Norra och Södra Norrland) är den jonosfäriska variationen större under natten än på dagtid, medan för de mer sydliga regionerna (Svealand och Götaland) är variationen större under dagtid. Vid maximal sol är variationen högre under månaderna mars, maj, september och oktober och mindre i juni, juli och augusti. För jonosfärens variationsprognos föreslås en modell baserad på Recurrent Neural Network (RNN) som kallas Long Short-Term Memory (LSTM). De inställda hyperparametrarna för LSTM testas med avseende på förutsägelsens noggrannhet genom att jämföra de förutsagda värdena med de uppmätta värdena. Det har visat sig att LSTM kan ge förutsägelsesresultaten med mer än 90% noggrannhet när man använder 1-6 timmars inmatningsdata och siktar på 10-35 minuters utdata. Längre varaktighet för in- och utgång resulterar i lägre noggrannhet för de förutsagda värdena.

Made available in DSpace on 2014-10-09T12:27:22Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:06:37Z (GMT). No. of bitstreams: 0 / Dissertacao (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP

Made available in DSpace on 2014-10-09T12:27:22Z (GMT). No. of bitstreams: 0 / Made available in DSpace on 2014-10-09T14:06:37Z (GMT). No. of bitstreams: 0 / Os nódulos de tireóide constituem patologia comum, com uma incidência entre 4- 7% na população brasileira. Embora a punção aspirativa por agulha fina (PAAF) seja um método com boa sensibilidade, a discriminação entre lesões benignas e neoplasias malignas não é possível em todos os casos, permitindo a incidência de diagnósticos falsos-positivos, o que conduz a tireoideotectomia pelo risco de carcinoma. O escopo deste estudo foi verificar se a espectroscopia de absorção no infravermelho por transformada de Fourier (FTIR) pode contribuir no diagnóstico diferencial entre neoplasias malignas e benignas de tecidos e aspirados. Amostras de PAAF, homogenatos e tecidos de nódulos de tireóide com o diagnóstico histopatológico foram obtidos e preparados para análise espectroscópica por FTIR. As punções e homogenatos foram medidas por -FTIR (entre 950 1750 cm-1, com resolução de 4 cm-1 e 120 varreduras). As amostras de tecido foram analisadas diretamente pela técnica de ATR-FTIR, com resolução de 2 cm-1, 60 varreduras, região entre 950 1750 cm-1.. Todos os espectros foram corrigidos pela linha base e normalizados pela área sob a banda das amidas (1550-1640 cm-1) de modo a minimizar as variações de homogeneidade das amostras. Os espectros foram então convertidos em segundas derivadas usando-se o filtro de Savitzk-Golay com 13 pontos na janela. A variância de Ward e distância euclidiana foram usadas para se processar a análise de clusters. As amostras de PAAF revelaram um complexo padrão espectral. Todas as amostras mostraram alguns aglomerados de células ou grande concentração de hormônios, tendo representação em algumas bandas em 1545 e 1655 cm-1. Foram também encontradas bandas em torno de 1409, 1412, 1414, 1578 and 1579 cm-1, indicando a possível presença de açúcares, DNA e ácido cítrico de produtos metabólitos. Neste estudo, foi obtida uma excelente separação entre bócio adenomatoso e neoplasias malignas para as amostras de tecido, com 100% de sensibilidade em determinado cluster, mas 67% no geral e 50% de especificidade. Nos homogenatos e aspirados este valor foi menor (76,2% de sensibilidade e 52,6% de especificidade) porque incluiu outros tipos de lesões. Para uma maior diferenciação das amostras de PAAF de padrão folicular, um maior número de amostras se faz necessário. Os resultados deste estudo sugerem que a espectroscopia FTIR pode ser útil na diferenciação de carcinomas da tiróide em amostras de tecidos. / Dissertacao (Mestrado) / IPEN/D / Instituto de Pesquisas Energeticas e Nucleares - IPEN-CNEN/SP

Basée sur la reconversion de la centrale solaire THEMIS (Pyrénées Orientales françaises) en télescope pour l'astronomie gamma, CELESTE est la première expérience à explorer le spectre électromagnétique entre 10 GeV et 300 GeV et à relier ainsi le domaine des satellites à celui des imageurs au sol. Ce domaine d'énergie est particulièrement important pour les pulsars. En effet, aucun des six pulsars gamma haute énergie détectés par EGRET n'a été détecté au sol. Deux modèles théoriques visent à expliquer la cassure des spectres observée entre 1 et 100 GeV : calotte polaire et cavité externe. Ceux-ci diffèrent toutefois en plusieurs points et une détection dans ce domaine d'énergie permettrait d'éclaircir la situation. Cette thèse regroupe les premiers travaux dédiés à l'étude des pulsars avec CELESTE, et plus particulièrement deux candidats : le pulsar du Crabe et PSR B1951+32. La recherche d'un signal pulsé sous-entend une analyse quelque peu différente de celle développée pour les sources continues. Une première étape a donc consisté en l'adaptation à CELESTE de la procédure de datation spécifique. Dans une seconde étape, l'objectif de ce travail a été de développer une analyse spécifique préservant les basses énergies où est attendu un éventuel signal. Ainsi, en se basant sur les acquis des analyses précédentes et sur les caractéristiques des gerbes électromagnétiques et hadroniques en dessous de 50 GeV, des critères de réjection particuliers ont pu être établis et appliqués aux données. Les résultats résident essentiellement dans l'établissement de nouvelle limites supérieures sur l'énergie de coupure basse des deux pulsars observés. Bien qu'insuffisants pour contraindre les modèles théoriques, ceux-ci restent d'un intérêt certain pour la physique de ces objets ne serait ce que parce qu'ils constituent les premières mesures réalisées dans cette gamme d'énergie. Un excès a malgré tout été observé sur le Crabe mais avec une significativité insuffisante. Cette indication de modulation présentant les propriétés attendues, elle a été traduite en terme de flux dans l'hypothèse d'un signal pulsé, puis interprétée. Si de nouvelles observations venaient a confirmer cet excès, il s'agirait de la première détection autour de 30 GeV et le modèle Polar Cap se verrait alors sérieusement remis en cause.