Orientador: Ernesto Kemp / Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin / Made available in DSpace on 2018-08-20T15:39:35Z (GMT). No. of bitstreams: 1 Batista_RafaelAlves_M.pdf: 8040703 bytes, checksum: 596e886c4828986af7fb003ba71adf9b (MD5) Previous issue date: 2012 / Resumo: Campos magnéticos cósmicos são ubíquos e estão presentes em todas as escalas, desde os planetas até os superaglomerados de galáxias. Sabe-se que o campo magnético da Via Láctea possui uma componente regular, que tem uma estrutura espiral, e uma componente aleatória. Muitas questões acerca do magnetismo galáctico ainda permanecem sem respostas, e o modelo de espiral mais adequado para descrever as observações é incógnito. Uma possibilidade pouco explorada para estudar o campo magnético da Via Láctea é utilização de informações relacionadas à propagação de partículas carregadas através da mesma. Neste contexto estão inseridos os raios cósmicos ultra-energéticos, as partículas mais energéticas do universo, cuja origem, composição química e mecanismos de aceleração e propagação não são bem compreendidos. A deflexão de partículas provenientes da mesma fonte no campo magnético galáctico pode gerar estruturas filamentares com eventos ordenados por energia, os chamados multipletos, sendo esta uma assinatura única deixada pelo campo em mapas contendo direções de chegada de raios cósmicos. Neste trabalho é apresentado um método inédito para estudos do campo magnético galáctico, através da identificação e análise da orientação de multipletos nestes mapas. Este método baseia-se na transformada de wavelets na esfera, que permite amplificar a razão sinal-ruído e fazer reconhecimento de padrões, de forma a identificar multipletos imersos em ruído de natureza estocástica. Na primeira parte do trabalho o método foi aplicado a dados simulados visando obter a orientação esperada para multipletos oriundos de fontes em diversas partes da esfera celeste, segundo diferentes modelos de campo magnético galáctico. Na segunda parte do trabalho, aplicou-se o método a eventos detectados pelo Observatório de Raios Cósmicos Pierre Auger. A confrontação dos resultados de dados reais e simulações permite restringir modelos de campo magnético galáctico / Abstract: Cosmic magnetic fields are ubiquitous and are present in all size scales, from planets to superclusters of galaxies. The magnetic field of the Milky Way has a regular component, with a spiral structure, and a random component. Many questions concerning galactic magnetism still remain unanswered, and the spiral model which best fits the observations is unknown. An underexplored possibility to probe these fields is to use information related to the propagation of charged particles through them. In this context, an interesting probe are the ultrahigh energy cosmic rays, the most energetic particles in the universe, whose origin, chemical composition and mechanisms of acceleration and propagation are not well-understood. The deflection of particles coming from the same source can generate threadlike structures with events ordered by energy, the so-called multiplets, which imprints a unique signature of the galactic magnetic field in maps containing arrival directions of cosmic rays. In the present work it is presented a novel method to probe the galactic magnetic field, by identifying and analysing the orientation of multiplets in these maps. This method relies on the spherical wavelet transform, which is capable of amplifying the signal-to-noise ratio and perform pattern matching, so that it is possible to identify multiplets embedded in a stochastic background. In the first part of this work the method is applied to simulated data, aiming to obtain the expected orientations for multiplets associated to sources in several regions of the celestial sphere, according to different models of galactic magnetic field. In the second part of the work the method was applied to events detected by the Pierre Auger Observatory. A confrontation between the results using real and simulated data allows one to impose constraints to galactic magnetic field models / Mestrado / Física / Mestre em Física

The dynamics of the solar corona are dominated by the magnetic field which creates its structure. The magnetic field in most of the corona is ‘frozen’ to the plasma very effectively. The exception is in small localised regions of intense current concentrations where the magnetic field can slip through the plasma and a restructuring of the magnetic field can occur. This process is known as magnetic reconnection and is believed to be responsible for a wide variety of phenomena in the corona, from the rapid energy release of solar flares to the heating of the high-temperature corona. The coronal field itself is three-dimensional (3D), but much of our understanding of reconnection has been developed through two-dimensional (2D) models. This thesis describes several models for fully 3D reconnection, with both kinematic and fully dynamic models presented. The reconnective behaviour is shown to be fundamentally different in many respects from the 2D case. In addition a numerical experiment is described which examines the reconnection process in coronal magnetic flux tubes whose photospheric footpoints are spun, one type of motion observed to occur on the Sun. The large-scale coronal field itself is thought to be generated by a magnetohydrodynamic dynamo operating in the solar interior. Although the dynamo effect itself is not usually associated with reconnection, since the essential element of the problem is to account for the presence of large-scale fields, reconnection is essential for the restructuring of the amplified small-scale flux. Here we examine some simple models of the solar-dynamo process, taking advantage of their simplicity to make a full exploration of their behaviour in a variety of parameter regimes. A wide variety of dynamic behaviour is found in each of the models, including aperiodic modulation of cyclic solutions and intermittency that strongly resembles the historic record of solar magnetic activity.

No description available.

No / A crucial challenge to successful flare prediction is forecasting periods that transition between "flare-quiet" and "flare-active." Building on earlier studies in this series in which we describe the methodology, details, and results of flare forecasting comparison efforts, we focus here on patterns of forecast outcomes (success and failure) over multiday periods. A novel analysis is developed to evaluate forecasting success in the context of catching the first event of flare-active periods and, conversely, correctly predicting declining flare activity. We demonstrate these evaluation methods graphically and quantitatively as they provide both quick comparative evaluations and options for detailed analysis. For the testing interval 2016-2017, we determine the relative frequency distribution of two-day dichotomous forecast outcomes for three different event histories (i.e., event/event, no-event/event, and event/no-event) and use it to highlight performance differences between forecasting methods. A trend is identified across all forecasting methods that a high/low forecast probability on day 1 remains high/low on day 2, even though flaring activity is transitioning. For M-class and larger flares, we find that explicitly including persistence or prior flare history in computing forecasts helps to improve overall forecast performance. It is also found that using magnetic/modern data leads to improvement in catching the first-event/first-no-event transitions. Finally, 15% of major (i.e., M-class or above) flare days over the testing interval were effectively missed due to a lack of observations from instruments away from the Earth-Sun line.

Wie seit schon einigen Jahrzehnten bekannt ist, werden akustische Oszillationen durch stellare Aktivität beeinflusst. Die globalen akustischen Moden in der Sonne weisen eine Variation mit dem 11-jährigen Sonnenzyklus auf. Ein ähnliches Phänomen konnte auch in anderen Sternen mit Hilfe von Asteroseismologie nachgewiesen werden. In dieser Arbeit erforsche ich den Einfluss von großen Sternflecken auf globale Oszillationen mit niedrigem Grad ℓ. Als wichtigstes Werkzeug benutze ich hierfür den GLASS Kode, der die Ausbreitung von linearen akustischen Wellen im Sterninneren in 3D simuliert. Zunächst habe ich das Problem der konvektiven Stabilisierung betrachtet, welches bei jedem linearen Oszillationskode im Zeitbereich auftritt. Ich präsentiere eine allgemeine Methode um konvektiv stabile Hintergrundsmodelle für ein vorgegebenes Sternmodell zu erzeugen. Dabei werden wichtige Eigenschaften des ursprünglichen Modells beibehalten, beispielsweise das hydrostatische Gleichgewicht. Ich schlage einen störungstheoretischen Ansatz vor, um das akustische Wellenfeld in dem ursprünglichen instabilen Sternmodell näherungsweise zu erlangen. Tests zeigen, dass für Moden mit niedrigem Grad ℓ und einer Frequenz um 3 mHz die korrigierten Frequenzen mit einer Genauigkeit von 1 μHz mit den exakten Werten übereinstimmen. Zweitens habe ich mit Hilfe des GLASS Kodes den Einfluss einer am Nordpol des Sterns lokalisierten Störung der Schallgeschwindigkeit auf radiale, dipolare und quadrupolare Oszillationsmoden untersucht. Diese Studie zeigt auf, dass die axialsymmetrischen Moden dadurch am stärksten beeinflusst werden und im Falle von großen Sternflecken können ihre Frequenzen nicht mit der linearen Theorie berechnet werden. Die Form der Eigenfunktionen der Moden weicht von reinen Kugelflächenfunktionen ab und werden mit Kugelflächenfunktionen mit unterschiedlichem Grad ℓ vermischt. Dies könnte die korrekte Identifikation der Moden in der spektralen Leistungsdichte beeinflussen. Drittens habe ich den beobachtbaren Einfluss eines großen Sternflecks auf Moden mit Grad ℓ betrachtet. Im Falle einer aktiven Region, die mit dem Stern rotiert (und sich nicht am Pol befindet), ist die Störung nicht stabil, wenn sie in einem Inertialsystem betrachtet wird. Der kombinierte Einfluss von Rotation und Sternfleck veranlasst jede Mode, in der beobachteten spektralen Leistungsdichte als (2ℓ + 1)² Peaks aufzutreten. Die Einhüllende der spektralen Leistungsdichte eines Multipletts ist also komplex und hängt von dem Breitengrad ab, wo sich die aktive Region befindet, und vom Inklinationswinkel des Sterns. Ich berechne die spektrale Leistungsdichte für einige Beispiele sowohl mit Störungstheorie als auch mit Hilfe von GLASS. Diese Arbeit soll dazu beitragen, die spektrale Leistungsdichte von oszillierenden Sternen, die Sternflecken aufweisen, zu interpretieren.

This thesis investigates a number of transition-metal coordination polymers and iron-pnictide superconductors through the use of high magnetic fields, low temperatures, and on occasion, high pressures. The thesis will begin by describing my development of the proximity detector dynamic susceptometer, a novel technique that can be used for magnetometery and transport measurements in high magnetic fields. This technique is highly compact and has no moving parts, making it suitable for use in pressure cells, hence opening the way for a variety of new experiments. Through high-field magnetometery and other measurements, I will demonstrate that the pressure can be used to directly control the magnetic properties of the polymeric magnet CuF₂(H₂O)₂(pyrazine). In particular, I observe a transition from quasi-two-dimensional to quasi-one-dimensional antiferromagnetism at 9~kbar, driven by the rotation of the Jahn-Teller axis. I will then present a series of measurements on two coordination polymers, showing how a small chemical difference can lead to drastically different magnetic properties. I show that [Cu(pyrazine)H₂O(glycine)₂]ClO₄ is an excellent spin-chain, while the sister compound [Cu(pyrazine)(glycine)]ClO₄ is a dimerised material that shows a spin-gap and is disordered down to very low temperatures, but then undergoes a field-induced phase transition to an ordered phase. I will also describe a series of pulsed-field measurements of the upper critical field of the iron-based superconductors NaFe_1-xCo_xAs across the whole of the doping phase diagram. It is shown that paramagnetic pair-breaking effects dominate the critical field when the field is parallel to the crystal planes. In the parent compound the paramagnetic limit is equal to that expected from BCS theory, but becomes significantly enhanced above the BCS limit upon doping. It is shown that the multi-band nature of the superconductivity leads to a convex curvature in the evolution of the critical field as the temperature is reduced.

No description available.

Thesis (PhD (Electrical and Electronic Engineering))--University of Stellenbosch, 2010. / ENGLISH ABSTRACT: Certain types of electric machines are particularly susceptible to the proliferation of eddy currents flowing within the solid conducting regions in the rotor. Single-layer, non-overlapping windings within uneven open slots are some stator properties that can produce damaging, asynchronous magnetic field harmonics which manifest in the rotor as eddy currents. The ohmic losses caused by these eddy currents are a source of inefficiency and can cause a marked increase in the temperature of the rotor. This temperature rise can be dangerous for the magnets, which have to be kept within temperature limits to avoid partial or full demagnetization. The research work presented here is concerned with reducing the effect of eddy currents in the rotor magnets and solid rotor yoke of an electric machine. The work presents analytical methods to calculate the magnetic fields, eddy currents and solid loss in an electric machine due to current in the winding and due to the interaction of the permeance variation in the stator with the magnets in the rotor. A method is also suggested where the analytical theory can be used with a magnetostatic finite element solution to produce a transient solid loss result. The research work also investigates a method for optimal segmentation in both level and penetration, and provides some design suggestions. The work presents the method of partial magnet segmentation, which is a technique whereby thin incisions are made into the magnet material from one or both sides. Another method of partial rotor segmentation is also presented where the incisions are made into a portion of the magnet-facing solid yoke. These methods attempt to interrupt the flow of eddy currents and increase the resistance ‘seen’ by the eddy currents, while also keeping construction difficulty and cost to a minimum. The methods are verified using finite element calculations which are compared to measured results. The result is that partial magnet segmentation is a very useful, effective and practical method of segmenting magnets. The loss reduction profile can be similar to that of traditional full segmentation. The method of partial rotor segmentation also shows a large reduction in rotor power loss. With implementation of these methods on a test machine, one can expect an efficiency increase of more than 4 % / AFRIKAANSE OPSOMMING: Sekere tipes van elektriese masjiene is veral sensitief vir die vloei van werwelstrome in solied geleidende gebiede in die rotor. Enkellaag, nie-oorvleuelende wikkelings in oneweredige oop gleuwe is enkele stator eienskappe wat skadelike, asinchrone magneetveld harmonieke tot gevolg kan hê, wat as werwelstrome in die rotor manifesteer. Die ohmiese verliese wat deur hierdie werwelstrome teweeg gebring word is 'n bron van ondoeltreffendheid en kan lei tot 'n merkbare toename in die temperatuur van die rotor. Hierdie temperatuur styging hou gevaar in vir die magnete en moet binne temperatuur limiete gehou word om gedeeltlike of self volle demagnetisering te vermy. Die navorsing vervat in hierdie document is gemoeid met die vermindering van die effek van werwelstrome in die rotor magnete en in die soliede rotor juk van 'n elektriese masjien. Die werk bied analitiese metodes aan vir die berekening van die magneetvelde, werwelstrome en soliede verliese in ’n elektriese masjien as gevolg van strome in die wikkelings en die interaksie van die permeansie variasie van die stator met die magnete in die rotor. ’n Metode word ook voorgestel waar die analitiese teorie saam met ’n magnetostatiese eindige element oplossing gebruik word om ’n resultaat vir die oorgang soliede verliese te verkry. Die navorsingswerk ondersoek ook ’n metode vir die optimale segmentering in beide vlak sowel as penetrasie, en verskaf sekere ontwerp voorstelle. Die werk bied die metode aan van gedeeltelike magneet segmentering, wat 'n tegniek is waarvolgens dun insnydings gemaak word aan een of beide kante van die magneet materiaal. Nog ’n metode van gedeeltelike rotor segmentering word beskou waar die insnydings in in ’n gedeelte aan die magneetkant van die soliede rotor juk gemaak word. Hierdie metodes poog om die vloei van werwelstrome te onderbreek en die weerstand soos "gesien" deur die werwelstrome te verhoog, terwyl konstruksie kompleksiteit en koste tot ’n minimum beperk word. Die metodes word bevestig deur eindige element berekeninge wat met gemete resultate vergelyk word. Die gevolg is dat gedeeltelike magneet segmentering 'n baie nuttige, doeltreffende en praktiese metode van die segmentering van magnete is. Die verliesverminderingsprofiel van gedeeltelike segmentering kan soortgelyk wees aan dit van tradisionele volle segmentering. Die metode van gedeeltelike rotor segmentering toon ook 'n groot afname in rotor drywingsverlies. Met die implementering van hierdie metodes op ’n toetsmasjien, kan ’n mens ’n verhoging in benuttingsgraad verwag van meer as 4 %

Οι ολοένα αυξανόμενες ενεργειακές απαιτήσεις των σημερινών κοινωνιών και το γεγονός ότι οι ηλεκτρικές συσκευές και εξοπλισμός έχουν γίνει αναπόσπαστο κομμάτι της καθημερινότητάς μας, έχει οδηγήσει στην αναγωγή του ηλεκτρισμού σε κοινωνικό αγαθό. Παρόλα αυτά, η υπερβολική του χρήση έχει προκαλέσει έντονες ανησυχίες στο κοινό, όσον αφορά τα ηλεκτρομαγνητικά πεδία που εκπέμπονται λόγω του εναλλασσόμενου ρεύματος. Η παρούσα εργασία αποσκοπεί να ξεδιαλύνει το «θολό τοπίο» γύρω από τις επιδράσεις των χαμηλόσυχνων ηλεκτρομαγνητικών πεδίων (δηλαδή τα εκπεμπόμενα πεδία από τις εγκαταστάσεις ηλεκτρικής ενέργειας και τις ηλεκτρικές συσκευές) στην ανθρώπινη υγεία κι έτσι να συνεισφέρει ως ένα βαθμό στην άρση των ανησυχιών του κοινού και των επιπτώσεων που αυτές συνεπάγονται. Ειδικότερα, η εργασία μπορεί να συνοψιστεί ως εξής: Στο Κεφάλαιο 1 γίνεται μια θεωρητική αναφορά στις βασικές έννοιες της ηλεκτρομαγνητικής ακτινοβολίας. Προσδιορίζονται οι επιβλαβείς ακτινοβολίες για την υγεία καθώς επίσης και οι ιδιότητες των χαμηλόσυχνων ηλεκτρομαγνητικών πεδίων. Ακόμη, παρουσιάζονται οι κανονισμοί προστασίας και τα όρια έκθεσης σε ηλεκτρομαγνητικά πεδία, τόσο στην Ευρώπη, όσο και στην Ελλάδα. Στο Κεφάλαιο 2 παρουσιάζονται αναλυτικά οι διαφορετικές πηγές χαμηλόσυχνων ηλεκτρομαγνητικών πεδίων και γίνεται σύγκριση των πεδιακών εντάσεων στο περιβάλλον τους. Στο Κεφάλαιο 3 γίνεται λόγος για τη βιολογική επίδραση των ηλεκτρομαγνητικών πεδίων. Παρουσιάζονται οι επιδράσεις τους στην ανθρώπινη υγεία και οι δράσεις που λαμβάνουν χώρα τόσο για τη μελέτη αυτών των επιδράσεων, όσο και για την προστασία του κοινού. Στο Κεφάλαιο 4 γίνεται ανασκόπηση του προτύπου λήψης μετρήσεων που ακολουθήθηκε. Εξετάζεται το πρότυπο ΙΕC 61786 για μέτρηση χαμηλόσυχνων ηλεκτρομαγνητικών πεδίων και αναφέρονται κάποια χαρακτηριστικά του προτύπου EN 50413 για μέτρηση ηλεκτρομαγνητικών πεδίων όλων των συχνοτήτων. Στο Κεφάλαιο 5 περιγράφεται ο σκοπός και ο εξοπλισμός των μετρήσεων. Παρατίθενται τα αποτελέσματα των μετρήσεων συνοδευόμενα με διαγράμματα και σχόλια επί της μεταβολής της μαγνητικής επαγωγής στο περιβάλλον σχολικών συγκροτημάτων. Τέλος συνοψίζονται τα συμπεράσματα που εξάγονται με βάση όσα εξετάστηκαν στην παρούσα εργασία. Σύμφωνα με αυτά δεν πρέπει να υπάρχει κανένας λόγος ανησυχίας για την επίδραση των χαμηλόσυχνων ηλεκτρομαγνητικών πεδίων στην ανθρώπινη υγεία, καθώς τηρούνται όλοι οι κανονισμοί, οι οποίοι εμπεριέχουν μεγάλους συντελεστές ασφαλείας. / The ever-increasing energy demands of today's society and the fact that electrical appliances and equipment have become an integral part of our daily lives has led to the deduction of electricity into social good. However, its excessive use has caused great concern to the public, regarding to electromagnetic fields’ emissions because of the AC current. This essay aims to unravel the "misty area" around the effects of low frequency electromagnetic fields (i.e. fields emitted from power systems and electrical appliances) to human health and thus contribute to some extent to the disentanglement of public preoccupations and the consequences arising therefrom. In particular, this essay can be summarized as follows: In Chapter 1 there is a theoretical report in the basic concepts of electromagnetic radiation. Harmful radiation as well as the properties of low frequency electromagnetic fields is identified. Moreover, protection regulations and limits on exposure to electromagnetic fields are presented, both in Europe and in Greece. In Chapter 2 different sources of low frequency electromagnetic fields are presented and the fields’ intensities in their environment are compared. Chapter 3 talks about the biological effects of electromagnetic fields. It also presents the effects on human health and the actions that take place for the study of these effects, and for the public’s protection. Chapter 4 gives an overview of the pattern of taking measurements that was followed. The IEC 61786 standard for measuring low frequency electromagnetic fields is examined and some features of the standard EN 50413 for measuring electromagnetic fields of all frequencies are presented. Chapter 5 describes the measurements’ purpose and equipment. The measurements’ results are given, which are accompanied by charts and comments about the change of the magnetic induction around school buildings. Finally, the conclusions based on this essay’s data are summed up, according to which, there should be no reason for public concern about the effect of low frequency electromagnetic fields on human health, since compliance with all special regulations, which contain large safety factors, is being performed.

Flux is continually emerging on the Sun, making its way from the solar interior up into the atmosphere. Emergence occurs on small-scales in the quiet Sun where magnetic fragments emerge, interact and cancel and on large-scales in active regions where magnetic fields emerge and concentrate to form sunspots. This thesis has been concerned with the large-scale emergence process and in particular the results from previous solar flux emergence modelling endeavours. Modelling uses numerical methods to evolve a domain representing simplified layers of the Sun’s atmosphere, within which the subsurface layer contains magnetic flux. The flux is initialised such that it will rises towards the surface at the start of the simulation. Once the flux reaches the solar surface, it can only emerge into the atmosphere if a magnetic buoyancy instability occurs, after which it expands rapidly both vertically and horizontally. The aim of this thesis is to test the robustness of these general findings from simulations to date upon the seed magnetic field. More explicitly, we have used three-dimensional numerical simulations to investigate how variations in the subsurface magnetic field modify the emergence process and the resulting atmospheric field. We initially consider a simple constant twist flux tube for the seed field and vary the tube’s magnetic field strength and degree of twist. Additionally, we have examined the effects of using non-constant twist flux tubes as the seed field by choosing two different profiles for the twist that are functions of the tube’s radius. Finally, we have investigated the effects of increasing the complexity of the seed field by positioning two flux tubes below the solar surface and testing two different configurations for the tubes. In both cases, the magnetic fields of the two tubes are such that, once the tubes come into contact with each other, reconnection occurs and a combined flux system is formed. From our investigations, we conclude that the general emergence results given by previous simulations are robust. However, for constant twist tubes with low field strength and twist, the buoyancy instability fails to be launched when the tubes reach the photosphere and they remain trapped in the low atmosphere. Similarly, when the non-constant twist profile results in a low tension force throughout the tube, we find that the buoyancy instability is not initialised.