Partitionierung von Graphen ist im Allgemeinen sehr schwierig. Es stehen derzeit keine Algorithmen zur Verfügung, die ein allgemeines Partitionierungsproblem effizient lösen. Aus diesem Grund werden heuristische Ansätze verfolgt. Zur Analyse dieser Heuristiken ist man derzeit gezwungen zufällige Graphen zu Verwenden. Daten realer Graphen sind derzeit entweder nur sehr schwer zu erheben (z.B. Internetgraph), oder aus rechtlichen bzw. wirtschaftlichen Gründen nicht zugänglich (z.B. soziale Netzwerke). Die untersuchten Heuristiken liefern teilweise nur unter bestimmten Voraussetzungen Ergebnisse. Einige arbeiten lediglich auf einer eingeschränkten Menge von Graphen, andere benötigen zum Erkennen einer Partition einen mit der Knotenzahl steigenden Durchschnittsgrad der Knoten, z.B. [DHM04]. Der im Zuge dieser Arbeit erstmals implementierte Algorithmus aus [CGL07a] benötigt lediglich einen konstanten Durchschnittsgrad der Knoten um eine Partition des Graphen, wenn diese existiert, zu erkennen. Insbesondere muss dieser Durchschnittsgrad nicht mit der Knotenzahl steigen. Nach der Implementierung erfolgten Tests des Algorithmus an zufälligen Graphen. Diese Graphen entsprachen dem Gnp-Modell mit eingepflanzter Partition. Die untersuchten Clusterprobleme waren dabei große Schnitte, kleine Schnitte und unabhängige Mengen. Der von der Art des Clusterproblems abhängige Durchschnittsgrad wurde während der Tests bestimmt.

Two of the principal phenomena observed and exploited in the field of spintronics are giant magnetoresistance (GMR) and spin transfer torque (STT). With GMR, the resistance of a magnetic multilayer is affected by the relative orientation of its magnetic layers due to (electron) spin dependent scattering. For the STT effect, a spin-polarized electric current is used to alter the magnetic state of a ferromagnet. Together, GMR and STT are at the foundation of numerous technologies, and they hold promise for many more applications. To achieve the high current densities (~10¹² A/m²) that are necessary to observe STT effects, point contacts – constricted electrical pathways (~1–100 nm in diameter) between conducting materials – are often used because of their small cross-sectional areas. In this sense, we have explored STT in bilayer magnetic nanopillars, where an electric current was used to induce precession of a ferromagnetic layer. This precessional state was detected as an increase in resistance of the device, akin to GMR. Temperature dependent measurements of the onset of precession shed light on the activation mechanism, but raised further questions about its detailed theory. Point contacts can also be used as local sources or detectors of electrons. In this context, we have observed transverse electron focusing (TEF) in a single crystal of bismuth. TEF is a k-selective technique for studying electron scattering from within materials. Using lithographically fabricated point contacts, we have studied the temperature dependence of the relaxation time for ballistic electrons from 4.2 to 100 K. These measurements indicated a transition between electron-electron dominated scattering at low temperatures and electron-phonon scattering as the Debye temperature was approached. We present preliminary work toward a TEF experiment to measure spin dependent scattering from a non-magnet/magnet interface. We also investigated spin wave propagation in thin, magnetic waveguide structures. At the boundary between the waveguide and continuous magnetic film, spin wave rays were found to radiate into the film, or to reflect and form standing waves in the waveguide. A circular defect in the waveguide was observed to cause diffraction of spin waves, generating an interference pattern of higher modes of oscillation. / text

The purpose of the thesis is to explore the role of BMP signaling in developing vertebrate midbrain. BMP signaling plays important roles in various tissues and stages of neural development to regulate cell fate, proliferation, differentiation, morphogenesis and more. We observed that several major BMPs are expressed not only at the roof plate but also the floor plate of the midbrain. This has led us to ask the role of BMP signaling in dorsal and ventral midbrain patterning. Despite ventral experiments, we found that BMP signaling does not regulate ventral cell fate specification in the midbrain. Instead BMPs profoundly influence the shape and early morphogenesis of the midbrain neural plate as it closes into a neural tube. During neural tube closure, one of the early events occurring at the ventral midline is median hinge point (MHP) formation. Failure to form MHP leads to neural tube closure defects, the 2nd most common birth defects in humans. However, the molecular mechanisms underlying MHP formation are not well known. We found that the lowest BMP signaling occurs at the MHP during early neurulation and BMP blockade is necessary and sufficient for MHP formation. Interestingly, we also demonstrated that BMP blockade directs MHP formation by regulating the apicobasal polarity pathway and this regulation may be mediated by biochemical interactions between pSMAD5 and the apical protein, PAR3. Additionally, our time-lapse data suggest that BMP blockade slows cell cycle progression by increasing duration of G1 to S transition and S phase which leads cell nuclei stay at the basal location longer. This mimics basal nuclear migration seen at the MHP where low BMP signaling occurs. Thus, we conclude that BMP signaling regulates neural tube closure via the apicobasal polarity pathway and in a cell cycle dependent manner at the ventral midline. We observed that BMP signaling is necessary and sufficient for the dorsal cell fate specification in a context-dependent manner and ventral BMP signaling affects dorsal cell fates. Taken together, we propose the idea that BMP signaling has distinct roles in different contexts. BMPs regulate tissue morphogenesis in the ventral midbrain and dorsally cell fate specification. / text

This thesis presents a starburst model for far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) line emission of molecular and atomic gas in an evolving starburst region, which is treated as an ensemble of non-interacting hot bubbles which drive spherical shells of swept-up gas into a surrounding uniform gas medium. These bubbles and shells are driven by winds and supernovae within massive star clusters formed during an instantaneous starburst. The underlying stellar radiation from the evolving clusters affects the properties and structure of photodissociation regions (PDRs) in the shells, and hence the spectral energy distributions (SEDs) of the molecular and atomic line emission from these swept-up shells and the associated parent giant molecular clouds (GMCs) contains a signature of the stage evolution of the starburst. The physical and chemical properties of the shells and their structure are computed using a a simple well known similarity solution for the shell expansion, a stellar population synthesis code, and a time-dependent PDR chemistry model. The SEDs for several molecular and atomic lines ($^{12}$CO and its isotope $^{13}$CO, HCN, HCO$^+$, C, O, and C$^+$) are computed using a non-local thermodynamic equilibrium (non-LTE) line radiative transfer model. By comparing our models with the available observed data of nearby infrared bright galaxies, especially M 82, we constrain the models and in the case of M 82, provide estimates for the age of the recent starburst activity. We also derive the total H$_2$ gas mass in the measured regions of the central 1 kpc starburst disk of M 82. In addition, we apply the model to represent various stages of starburst evolution in a well known sample of nearby luminous infrared galaxies (LIRGs). In this way, we interpret the relationship between the degree of molecular excitation and ratio of FIR to CO luminosity to possibly reflect different stages of the evolution of star-forming activity within their nuclear regions. We conclude with an assessment of the strengths and weaknesses of this approach to dating starbursts, and suggest future work for improving the model.

This thesis presents a starburst model for far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) line emission of molecular and atomic gas in an evolving starburst region, which is treated as an ensemble of non-interacting hot bubbles which drive spherical shells of swept-up gas into a surrounding uniform gas medium. These bubbles and shells are driven by winds and supernovae within massive star clusters formed during an instantaneous starburst. The underlying stellar radiation from the evolving clusters affects the properties and structure of photodissociation regions (PDRs) in the shells, and hence the spectral energy distributions (SEDs) of the molecular and atomic line emission from these swept-up shells and the associated parent giant molecular clouds (GMCs) contains a signature of the stage evolution of the starburst. The physical and chemical properties of the shells and their structure are computed using a a simple well known similarity solution for the shell expansion, a stellar population synthesis code, and a time-dependent PDR chemistry model. The SEDs for several molecular and atomic lines ($^{12}$CO and its isotope $^{13}$CO, HCN, HCO$^+$, C, O, and C$^+$) are computed using a non-local thermodynamic equilibrium (non-LTE) line radiative transfer model. By comparing our models with the available observed data of nearby infrared bright galaxies, especially M 82, we constrain the models and in the case of M 82, provide estimates for the age of the recent starburst activity. We also derive the total H$_2$ gas mass in the measured regions of the central 1 kpc starburst disk of M 82. In addition, we apply the model to represent various stages of starburst evolution in a well known sample of nearby luminous infrared galaxies (LIRGs). In this way, we interpret the relationship between the degree of molecular excitation and ratio of FIR to CO luminosity to possibly reflect different stages of the evolution of star-forming activity within their nuclear regions. We conclude with an assessment of the strengths and weaknesses of this approach to dating starbursts, and suggest future work for improving the model.

ν Octantis is a spectroscopic binary with a semi-major axis and period of 2.55 AU and 2.9 years, respectively. Ramm et al. (2009) discovered a 52 ms^(-1) radial-velocity (RV) perturbation with a period of 417 days in this system. All evidence, both photometric and spectroscopic, suggests the perturbation is the result of a 2.5 MJ planet orbiting the primary star. However, when assuming a “normal” prograde coplanar orbit, celestial mechanics predicts this orbit is unstable, contradicting the observed stability. Simulations by Eberle and Cuntz (2010) showed a retrograde orbit for the planet to be stable for at least 10^7 years. In this thesis, we performed a 10^8 -yr simulation of the retrograde orbit, and found it remained stable. Simulations over a range of planetary semi-major axes, eccentricities, and primary/secondary masses showed that stable retrograde orbits are not possible past a semi-major axis of 1.315 +/- 0.092 AU . Therefore, planetary retrograde orbits are most likely inherently more stable than prograde orbits owing to the absence of stability at known mean-motion resonances. Eccentricity simulations showed that the period of the planet's dominant eccentricity variation is related to the planet's semi-major axis by a second order exponential. However, retrograde orbits tend to have longer eccentricity periods than prograde orbits at the same semi-major axis. There is also evidence that this eccentricity period is connected to the orbital stability. By fitting a keplerian to both Ramm et al. (2009) and current radial velocities, the period of the ν Octantis binary was determined to be 1050.04 +/- 0.02 days with an eccentricity of 0.2359 +/- 0.001 . The planetary orbital solution for just the data reduced in this thesis gave a period of 416.9 +/- 2.1 days and an eccentricity of 0.099 +/- 0.015 , with an RMS scatter of 9.6 ms^(-1). Therefore, the orbital elements are within 1σ of the Ramm et al. (2009) elements. Assuming a retrograde coplanar orbit about the primary star then the planet has a mass of M_pl = 2.3 M_J and a semi-major axis of a_pl = 1.21 +/- 0.09 AU.

Giant molecular clouds (GMCs), out of which stars form, are complex, dynamic systems, which both influence and are shaped by the process of star formation. In this dissertation, I examine three different facets of the dynamical motions within GMCs. Collapse modes in different dimensional objects. Molecular clouds contain lower dimensional substructures, such as filaments and sheets. The collapse properties of finite filaments and sheets differ from those of spherical objects as well as infinite sheets and filaments. I examine the importance of local collapse modes of small central perturbations, relative to global collapse modes, in different dimensional objects to elucidate whether strong perturbations are required for molecular clouds to fragment to form stars. I also calculate the dependence of the global collapse timescale upon the aspect ratio of sheets and filaments. I find that lower dimensional objects are more readily fragmented, and that for a constant density, lower dimensional objects and clouds with larger aspect ratios collapse more slowly. An edge-driven collapse mode also exists in sheets and filaments and is most important in elongated filaments. The failure to consider the geometry of a gas cloud is shown to lead to an overestimation of the star formation rate by up to an order of magnitude. Molecular tracers of turbulent energy dissipation. Molecular clouds contain supersonic turbulence that simulations predict will decay rapidly via shocks. I use shock models to predict which species emit the majority of the turbulent energy dissipated in shocks and find that carbon monoxide, CO, is primarily responsible for radiating away this energy. By combining these shock models with estimates for the turbulent energy dissipation rate of molecular clouds, I predict the expected shock spectra of CO from molecular clouds. I compare the results of these shock models to predictions for the emission from the unshocked gas in GMCs and show that mid-to-high rotational transitions of CO (e.g., J = 8 to 7), should be dominated by shocked gas emission and should trace the turbulent energy being dissipated in molecular clouds. Orion-Eridanus superbubble. The nearby Orion star forming region has created a large bubble of hot plasma in the local interstellar medium referred to as the Orion-Eridanus superbubble. This bubble is unusual in that it is highly elongated, is believed to be oriented roughly parallel to the galactic plane, and contains bright filamentary features on the Eridanus side. I fit models for a wind driven bubble in an exponential atmosphere to the Orion-Eridanus superbubble and show that the elongation of the bubble cannot be explained by such a model in which the scale height of the galactic disk is the typical value of 150 pc. Either a much smaller scale height must be adopted or some additional physics must be added to the model. I also show that the Eridanus filaments cannot be equilibrium objects ionized by the Orion star forming region. / Graduate / 0606 / andyrpon@gmail.com

Smart cards are widely used in different areas of modern life including identification, banking, and transportation cards. Some types of cards are able to store data and process information as well. A number of them can run cryptographic algorithms to enhance the security of their transactions and it is usually believed that the information and values stored in them are completely safe. However, this is generally not the case due to the threat of the side channel. Side channel analysis is the process of obtaining additional information from the internal activity of a physical device beyond that allowed by its specifications. There exist different techniques to attempt to obtain information from a cryptosystem using other ways than the normally permitted. This thesis presents a series of experiments intended to study the side channel from a particular type of smart card, known as Java Cards. This investigation uses the well known technique, Correlation Analysis, and a new type of side channel attack called fast correlation in the frequency domain to study the side channel of Java Cards. This research presents a giant magnetoresistor (GMR) probe and for the first time, this type of sensor is used to investigate the side channel. A novel setup designed for studying the side channel of smart cards is described and two metrics used to evaluate the analysis results are presented. After testing the GMR probe and methodology on electronic devices executing the Advanced Encryption Standard (AES), such as 8 bit microcontrollers and 128 bit AES implementations on FPGAs, these techniques were applied to analyse two different models of Java Cards working in the contactless mode. The results show that successful attacks on a software implementation of AES running on both models of Java Cards are possible.

Made available in DSpace on 2014-06-11T19:30:31Z (GMT). No. of bitstreams: 0 Previous issue date: 2009-02-19Bitstream added on 2014-06-13T20:21:12Z : No. of bitstreams: 1 guerreroalvarado_ce_dr_jabo.pdf: 1587825 bytes, checksum: 858924033c64c664e74d155a80686b1a (MD5) / Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) / Universidade Estadual Paulista (UNESP) / La formulation d’un régime alimentaire équilibré que puisse répondre aux besoins de calcium et de phosphore des larves de Macrobrachium rosenbergii est très important pour assurer des meilleures productivités à la fin de la larveculture. L’effet de différents niveaux de calcium et de phosphore sur le régime alimentaire a été evalué sur les principaux variables de production. Une délineation complétement au hasard en schème factoriel 3x3, a été utilisé, en correspondant à trois niveaux de calcium (0,35; 1,00 et 1,90%) et trois niveaux de phosphore (0,70; 1,50 et 2,30%). Chaque traitement a eu 3 répétitions. Deux jours après l’éclosion les larves ont été nourries avec des quantités croissantes de nauplii d’Artemia. A partir du onzième jour (zoea VII), la coalimentation a été introduite en fournissant les diètes-teste en plus des nauplii d’ Artemia jusqu’à la fin du cycle de larveculture. Au 27ème jour du cycle où 90% des larves, à peu près, se sont déjà méthamorphosées en pos-larves (PL), la récolte de fin d’élevage a été faite. Le taux de survie, la biomasse finale de PL, la pourcentage de larves et la productivité (PL L-1) ont été calculés pour chaque traitement. On a pu observer que les larves de M. rosenbergii qu’ont été nourries par une diète inerte de 0,35 ou 1,07% de calcium total et 1,50% de P total (1,15% de P disponible) ont eu leurs taux le survie beaucoup ameliorés aussi bien que le numero de pos-larves qu’ont été produites par litre à la fin da la larveculture. L’inclusion de 1% de P sur la forme de NaH2PO4 et le Ca venu de la diète basal (0,35%) sont suffisants pour améliorer la production de cette espèce. / A formulação de uma dieta balanceada que atenda as exigências dos minerais cálcio e fósforo nas larvas de Macrobrachium rosenbergii, é importante para garantir maior produtividade na larvicultura. Assim, avaliou-se o efeito de diferentes níveis de cálcio e fósforo na dieta sobre as principais variáveis de produção. O delineamento experimental foi em blocos casualizados, em esquema fatorial 3x3, correspondente a três níveis de cálcio (0,35; 1,00 e 1,90%) e três de fósforo (0,70; 1,50 e 2,30%), com três repetições realizadas em blocos temporais. Dois dias após a eclosão, as larvas passaram a ser alimentadas com quantidades crescentes de náuplios de Artemia. A partir do 11º dia (zoea VII), iniciou-se a co-alimentação, fornecendo-se as dietas-teste juntamente com os náuplios de Artemia até o final do ciclo de larvicultura. No 27º dia de cultivo, quando aproximadamente 90% das larvas metamorfosearam-se em pós-larvas (PL), realizou-se a despesca. Foi calculada a taxa de sobrevivência, a biomassa final de PL, a porcentagem de larvas e a produtividade (PL L-1) em cada tratamento. Observou-se que as larvas de M. rosenbergii alimentadas com dieta inerte contendo 0,35 ou 1,07% de Ca total, e 1,50% de P total (1,15% de P disponível) melhoraram significativamente a sobrevivência e o número de pós-larvas produzidas por litro ao final da larvicultura. A inclusão de 1% de P na forma de NaH2PO4 e unicamente o Ca proveniente da dieta basal (0,35%) são adequados para melhorar o desempenho produtivo desta espécie. / The formulation of a balanced diet, which provides the requirements of calcium and phosphorus minerals for Macrobrachium rosenbergii larvae is important to guarantee good productivity of post-larvae. Hence, the effect of different levels of calcium and phosphorus in the inert diet on the principal production variables was evaluated during the hatchery. It was used a randomized block experimental design, in a 3x3 factorial scheme, with three levels of calcium (0.35; 1.00 and 1.90 %) and three levels of phosphorus (0.70; 1.50 and 2.30 %), with three replicates. Two days after hatching, larvae started feeding on increasing quantities of Artemia nauplii. Co-feeding started at the 11th day (zoea VII), when test-diets plus Artemia nauplii were supplied up to the end of the rearing cycle. In the 27th day, when approximately 90% of the larvae turned into post larvae (PL), harvest was done. Survival rate, final biomass of PL, percentage of larvae and productivity (PL L-1) were calculated in all treatments M. rosenbergii larvae fed on inert diet containing 0.35 or 1.07 % of total Ca and 1.50 % of total P (1.15 % of P available) had significantly improved survival rate and productivity. Inclusion of 1.0 % of total P and only the dietary Ca from the basal diet (0.35%) are adequate to improve the productive performance on this specie. / La formulación de una dieta balanceada que atienda las exigencias de los minerales calcio y fósforo en las larvas de Macrobrachium rosenbergii, es importante para garantizar mejor productividade en la larvicultura. Asi, se evaluó el efecto de diferentes niveles de calcio y fósforo en la dieta sobre las principales variables de producción. El diseño experimental fue en bloques completamente al azar, en esquema factorial 3x3, correspondiente a tres niveles de calcio (0,35; 1,00 e 1,90%) y tres de fósforo (0,70; 1,50 e 2,30%), con tres repeticiones realizadas en bloques temporales. Dos días después de la eclosión las larvas pasaron a ser alimentadas con cantidades crecientes de náuplios de Artemia. A partir del 11º día (zoea VII), se inició la alimentación conjunta, ofreciendo las dietas-teste acompañadas por los náuplios de Artemia hasta el final del ciclo de larvicultura. El 27º día del cultivo, cuando aproximadamente 90% de las larvas se metamorfosearon en postlarvas (PL), se realizó la cosecha. Fue calculada la tasa de sobrevivencia, biomasa final de PL, el porcentaje de larvas y la productividad (PL L-1) en cada tratamiento. Se observó que las larvas de M. rosenbergii alimentadas con dieta inerte conteniendo 0,35 ó 1,07% de Ca total, y 1,50% de P total (1,15% de P disponible) mejoraran significativamente la sobrevivencia y el número de postlarvas producidas por litro al final de la larvicultura. La inclusión de 1% de P en la forma de NaH2PO4 y únicamente el Ca proveniente de la dieta basal (0,35%) son adecuados para mejorar el desempeño productivo de esta especie.

[pt] Elementos sensores baseados no efeito GMI são uma nova família de sensores magnéticos que apresentam grande quando submetidos a campos magnéticos externos. Estes sensores têm sido utilizados no desenvolvimento de magnetômetros de alta sensibilidade, destinados à medição de campos ultra fracos. Por sua vez, a sensibilidade de um magnetômetro está diretamente associada à sensibilidade de seus elementos sensores. No caso de amostras GMI, esta sensibilidade é otimizada buscando-se a maximização da variação do módulo ou da fase da impedância em função do campo magnético ao qual a amostra é submetida. Estudos recentes mostram que transdutores GMI baseados na variação de fase podem exibir sensibilidades até 100 vezes superiores às apresentadas por transdutores baseados na leitura do módulo do elemento sensor, o que fez com que os trabalhos conduzidos nesta dissertação focassem na maximização da sensibilidade de fase, a qual é majoritariamente dependente de quatro fatores: o comprimento da amostra, o campo magnético externo, o nível DC e a frequência da corrente de excitação. Contudo, a busca do conjunto de parâmetros que otimiza a sensibilidade das amostras é geralmente empírica e muito demorada. Esta dissertação propõe uma nova técnica de otimização da sensibilidade, baseada no uso de algoritmos genéticos evoluindo em hardware, a fim de se definir qual o conjunto de parâmetros responsável pela maximização da sensibilidade das amostras. Ressalta-se que, além dos parâmetros de otimização anteriormente explicitados, também foram realizados testes considerando a amplitude da corrente de excitação como uma variável livre, sendo que os resultados obtidos são apresentados e discutidos. Foi implementada uma bancada de testes e desenvolvida uma interface gráfica em LabVIEW, para monitorar e medir o comportamento da impedância de amostras GMI em função de variações nos parâmetros de interesse. Por sua vez, implementou-se um módulo de otimização em Matlab, baseado em algoritmos genéticos, responsável por encontrar a combinação de parâmetros que maximiza a sensibilidade dos sensores GMI avaliados (ponto ótimo de operação). / [en] GMI sensors are a new family of magnetic sensors that exhibit a huge variation of their impedance when subjected to external magnetic fields. These sensors have been used in the development of high sensitivity magnetometers, aimed at measuring ultra-weak magnetic fields. In turn, the sensitivity of a magnetometer is directly associated with the sensitivity of their sensor elements. In the case of GMI samples, this sensitivity is optimized by maximizing the variation of the impedance magnitude or phase as a function of the magnetic field applied to the sample. Recent studies show that GMI transducers based on phase variation can exhibit sensitivities up to 100 times higher than those presented by transducers based on impedance magnitude readings. The results obtained in these previous studies made the current work focusing on the maximization of phase sensitivity, which is mostly dependent on four factors: sample length, external magnetic field, DC level and frequency of the excitation current. However, the search for the set of parameters that optimizes the sensitivity of the samples is usually empirical and very time consuming. Thus, this dissertation proposes a new optimization technique, based on the use of genetic algorithms evolving on hardware, in order to define which set of parameters is responsible for maximizing the sensitivity of the samples. It should be noted that in addition to the optimization parameters previously described, this work also carried out tests considering the amplitude of the excitation current as a free variable, and the results obtained are presented and discussed. A test bench was implemented and a graphical interface was developed in LabVIEW to monitor and measure the impedance behavior of GMI samples due to variations in the parameters of interest. In turn, a Matlab optimization module based on genetic algorithms was implemented, in order to find the combination of parameters that maximizes the impedance phase sensitivity of the evaluated GMI sensors (optimum operating point).