This dissertation purposes to answer the question of whether or not the verb system of Black English in Dallas has the same features as those that characterize Black English in other sections of the country. Specifically, it describes in detail the use of the verb "be" within the speech of blacks in the Dallas metropolitan area and accounts for these usages formally within the framework of a transformational-generative grammar of the type proposed by Noam Chomsky.

We present Gemini Planet Imager polarized intensity imagery of HD 100453 in Y, J, and K1 bands that reveals an inner gap (9-18 au), an outer disk (18-39 au) with two prominent spiral arms, and two azimuthally localized dark features that are also present in Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) total intensity images. Spectral energy distribution fitting further suggests that the radial gap extends to 1 au. The narrow, wedge-like shape of the dark features appears similar to predictions of shadows cast by an inner disk that is misaligned with respect to the outer disk. Using the Monte Carlo radiative transfer code HOCHUNCK3D, we construct a model of the disk that allows us to determine its physical properties in more detail. From the angular separation of the features, we measure the difference in inclination between the disks (45 degrees) and their major axes, PA = 140 degrees east of north for the outer disk, and 100 degrees for the inner disk. We find an outer-disk inclination of 25 degrees +/- 10 degrees from face-on, in broad agreement with the Wagner et al. measurement of 34 degrees. SPHERE data in J and H bands indicate a reddish disk, which indicates that HD 100453 is evolving into a young debris disk.

Be stars are main-sequence stars and a specific subclass of B type stars with the unique characteristic of showing HI Balmer emission lines in their optical spectra that originates from a circumstellar disk around the star. Over the past 50 years, the Galactic Be star $\\omega$ CMa has exhibited quasi-regular outbursts, every 8 years or so, when the star brightens by about half a magnitude in the V-band. During these outbursts a new disk is formed during the first 3-4 years, and then dissipates in the following 4-6 years. We have access to a rich dataset (including photometry, polarimetry, interferometry and spectroscopy) of $\\omega$ CMa since March 1964 covering several outbursts and quiescence phases. Thus, nature has provided us the perfect experiment to study how Be star disks grow and dissipate. There is an increasing body of evidence that suggests that Be disks are well described by the Viscous Decretion Disk (VDD) model according to which the formation and structure of the disk depend on the kinematic viscosity of the gas. However, most observational tests of the VDD to-date were done for systems that do not display strong temporal variability. We use the rich dataset available for $\\omega$ CMa to perform the first in-depth test of the VDD scenario in a system with strong temporal variability. We use the radiative transfer code HDUST to analyze and interpret the observational dataset. From this analysis we (1) obtain a realistic physical model of the circumstellar environment; (2) measure the viscosity parameter of the gas, both during the formation and dissipation phases of the disk; (3) obtain a reliable estimate of the stellar mass and angular momentum loss rates during outburst. Our simulations offer a good description of the photometric variability, which suggests that the VDD model adequately describes the structural evolution of the disk. Furthermore, our analysis allowed us to determine the viscosity parameter $\\alpha$, as well as the net mass and angular momentum (AM) loss rates. We find that $\\alpha$ is variable, ranging from 0.1 to 1.0, not only from cycle to cycle but also within a given cycle. Additionally, build-up phases have larger values of $\\alpha$ than the dissipation phases. We also find that, contrary to what is generally assumed, during dissipation the outward AM flux is not necessarily zero, meaning that $\\omega$ CMa does not experience a true quiescence but, instead, switches between a high AM loss rate state to a low AM loss rate one during which the disk quickly assumes an overall lower density but never zero. We confront the average AM loss rate with predictions from stellar evolution models for fast-rotating stars, and find that our measurements are smaller by more than one order of magnitude. The model developed using the V-band photometry as a constraint was applied to several other observables. Overall, the results of this multi-technique study were very positive, with a good match for multi-band photometry, polarization, and most spectroscopic characteristics. This is a very relevant result, as it proves that a model that was constructed from constraints only from the very inner part of the disk (the $V$-band light curve), could be extended to the whole disk and to other physical processes. / Estrelas Be são um subtipo específico de estrelas de sequência principal de tipo espectral B. Elas possuem características únicas tais como a presença de linhas de emissão em seu espectro, que se originam de um disco circunstelar. Nos últimos 50 anos, a estrela Be galáctica CMa exibiu erupções quasi-regulares, a cada 8 anos aproximadamente, onde a estrela torna-se mais brilhante na banda V. Nestas erupções um novo disco se forma nos primeiros 3-4 anos e depois dissipa-se nos 4-6 anos seguintes. Temos acesso a uma base de dados rica (incluindo fotometria, polarimetria, interferometria e espectroscopia) de CMa desde março de 1964, que cobre vários ciclos de erupções e quiescências. Assim, a natureza nos proveu um experimento perfeito para estudar como discos de estrelas Be crescem e dissipam-se. Há um corpo de evidências cada vez maior que sugerem que os discos de estrela Be são bem descritos pelo modelo de decréscimo viscoso (VDD), segundo o qual a formação e estrutura do disco depende da viscosidade cinemática do gás. Entretanto, a maioria dos testes conduzidos com o VDD até o momento foram feitos para sistemas que não mostram forte variabilidade temporal. Usamos a rica base de dados de CMa para conduzir o primeiro teste aprofundado do VDD em um sistema fortemente variável. Usamos o código de transporte radiativo HDUST para analisar e interpretar os dados. Desta análise obtemos (1) um modelo fisicamente realista do ambiente circunstelar, (2) a viscosidade do gás, e (3) uma estimativa confiável das taxas de perda de massa e momento angular durante os eventos de formação do disco. Nossas simulações conseguem reproduzir a variabilidade fotométrica muito bem, o que sugere que o modelo VDD descreve corretamente a evolução estrutural do disco. Mostramos que o parâmetro de viscosidade é variável, com valores entre 0.1 e 1. Adicionalmente, as fases de construção do disco têm valores de viscosidade maior. Contrariamente ao que se acredita, mostramos que durante a dissipação a taxa de perda de momento angular não é necessariamente nula, o que implica que CMa não experimenta uma quiescência verdadeira, mas alterna entre uma fase de alta taxa de perda de momento angular (erupção) e uma fase de baixa taxa (quiescência). Confrontamos as taxas de perda de momento angular com as preditas pelos modelos evolutivos de Genebra, e encontramos que nossas taxas são mais que 10 vezes menores que as taxas de previstas pelos modelos. O modelo desenvolvido para reproduzir a curva de luz na banda V foi aplicado a vários outros observáveis. De forma geral, os resultados deste estudo multi-técnica foram muito positivos, com uma boa concordância com a fotometria multi-banda, polarização, e a maioria das características espectrais. Este é um resultado muito relevante, pois prova que um modelo que foi construído apenas a partir de vínculos para a interna do disco (a curva de luz na banda V), pode ser estendido para todo o disco e também outros processos físicos.

This thesis examines the Swedish Government Cyber Security Strategy laid out for the years 2016-2022 using Carol Bacchi’s discourse method and theory concept “What’s the problem represented to be” (WPR). The theoretical framework of the thesis also builds on critical theories on security- and threat perception following the concept of “exceptionalist securitising” and “diffusing insecurities”. The study suggests that the government has a national security focus that stresses “high politics” cyber threats rather than risks related to individuals and the Swedish society. Potential enemies are presented as located outside of the national boarders indicating a more traditional security perspective and enemy construction coming from other states. The study also disclosed that the strategy strives to stress the necessity of raising the awareness on cyber security as well as uniting the authorities working on cyber security while neglecting the democratic limits that political actions such as state-monitoring and data surveillance implicates.

Made available in DSpace on 2015-03-04T21:02:10Z (GMT). No. of bitstreams: 0 Previous issue date: 30 / Milton Valente / A presente pesquisa tem por objetivo legitimar o conceito de forma como belo em Lima Vaz. Principio de legitimidade filosófica que escapa a forma do belo, e é justamente por isso, por se encontrar nas dimensões da eternidade é que podemos falar da forma do belo em Lima Vaz. Forma é ser. Ou melhor, sendo formas o ser está enquanto “ens”. Assim, sendo-no-mundo a forma é aquilo que recebe tal condição do ser (Esse). Há, portanto, uma humildade ontológica da forma em receber e uma generosidade do ser em dar. Dizemos que a Forma não é ser, mas antes, “habens esse”, i. é, portadora do existir. Enquanto são portadoras do existir ou Esse, as formas são substâncias separadas. Constituídas por matéria que as individualiza e forma, i. é, o que assegura a substância ser o que ela é. Doravante, a substância - “algo que é” – é numa infinitude sensível, não o sensível meramente dos sentidos, mas anterior a este numa “unidade ontológica concreta” com o Esse. Sensível é perceber essa unidade concreta do ser. Dizer o “homem ex / This research aims to legitimize the concept os shape as beautiful in Lima Vaz. Philosophical principle of legitimacy that escapes the shape of beautiful, and is precisely why, because it was the size of eternity we can talk about the beautiful shape in Lima Vaz. Shape is to be. Or better, Shape as to be is “ens”. Therefore, being in the world as shape it´s receiving such a condition of being (Esse). There´s, thus a shape of ontological humility in receiving and a generosity in giving to be. We say that shape is not to be, but rather, “habens esse”, is the carrier exist. While there are carriers of to be or Esse, the shapes are separates substances. Consist of matters that individually and shapes, is what provides the substance is what it´s. Henceforth, the substance – “somethings that to be” – is an infinit sensitive, sensitive not only of the senses, but prior to that in a “concrete ontological unity” with this. Sensitive realize is that unit´s be concret. . Sayng the “man exist” is considering this singu

Submitted by Filipe dos Santos (fsantos@pucsp.br) on 2016-08-16T13:34:29Z No. of bitstreams: 1 Luciana de Paula Assis Ferriani.pdf: 2495470 bytes, checksum: 4d16847b07895aaa3e469e97acdd6778 (MD5) / Made available in DSpace on 2016-08-16T13:34:29Z (GMT). No. of bitstreams: 1 Luciana de Paula Assis Ferriani.pdf: 2495470 bytes, checksum: 4d16847b07895aaa3e469e97acdd6778 (MD5) Previous issue date: 2016-04-26 / Pontifícia Universidade Católica de São Paulo / The right to be forgotten is a topic that is as yet relatively unexamined in Brazilian law, but it has sparked the interest of the legal community. Recent decisions on the matter handed down by the Superior Court of Justice and also the Federal Supreme Court in Brazil have attracted attention. This paper situates the right to be forgotten as one of the personality rights. Additionally, it addresses the issue of the conflict between the right to be forgotten and other personality rights. Also discussed are various problems inherent to the topic that generate conflicts, both apparent and actually existing, between what the Brazilian Civil Code and Federal Constitution prescribe and the ancillary legislation. Based on research of numerous legal opinions, both Brazilian and foreign, as well as the jurisprudence, criticisms and suggestions are offered. For a full understanding of the matter, it was also necessary to discuss the topics of the right to the truth and the right to memory, to establish a parallel with the right to be forgotten. Finally, the criterion of weighting is presented for delineating the situations where the right to be forgotten may or may not be applied / O direito ao esquecimento é tema ainda pouco estudado no direito brasileiro, mas tem despertado o interesse da comunidade jurídica. Recentes acórdãos proferidos no Superior Tribunal de Justiça e também no Supremo Tribunal Federal, sobre o assunto, chamaram a atenção. O presente estudo enquadra o direito ao esquecimento como um dos direitos da personalidade. Além disso, desenvolve a questão relativa ao conflito entre o direito ao esquecimento com outros direitos da personalidade. Analisam-se diversos problemas ligados ao assunto, que geram conflitos, aparentes e efetivamente existentes, entre o que prescreve o Código Civil brasileiro, a Constituição Federal, e a legislação extravagante. A partir de pesquisa de inúmeras opiniões doutrinárias, nacionais e estrangeiras, além de jurisprudencial, são apresentadas críticas e sugestões. Para a compreensão do tema, foi necessário desenvolver, ainda, o tema do direito à verdade e do direito à memória para, assim, poder traçar um paralelo com o direito ao esquecimento. Por fim, foi apresentado o critério da ponderação para delimitar as situações em que o direito ao esquecimento poderá ou não ser aplicado

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / A presente dissertação tem por objeto o tema da negatividade ontológica constitutiva da existência humana na obra Ser e Tempo de Martin Heidegger. Na primeira parte é analisada as descrições efetuadas por Heidegger na primeira seção de Ser e Tempo sobre a dinâmica existencial do homem compreendido como ser-aí (Dasein). Nesse primeiro momento é evidenciado o caráter negativo da existência. Para tanto, partiremos da reconstrução dos conceitos de existência e deu seu caráter intencional e poder-ser (Seinkonnen) em Ser e Tempo. Na segunda parte, a análise da tonalidade afetiva da angústia é o ponto de partida para se chegar ao modo de ser do homem, descrito por Heidegger como cuidado (Sorge). Argumentaremos também, que o cuidado é o único modo de ser compatível com um ente que em seu modo de ser mais próprio é marcado por uma negatividade (incompletude) radical. Por último, em nosso terceiro capítulo, apresentaremos, em seus traços gerais, a possibilidade compatível com o caráter de poder-ser do ser-aí: a possibilidade da morte, compreendida ontologicamente como ser-para-a-morte. Na conclusão, apontaremos o interesse maior de Heidegger em investigar a dinâmica existencial do ser-aí. Esse interesse consiste, em visualizar, por meio do que Heidegger chama de crise existencial do ser-aí (proporcionada pela angústia) o ponto de gênese das ontologias. / The present dissertation aims the theme of ontological negativity constitutive of human existence in the work Being and Time of Martin Heidegger. In the first part, we examine the descriptions made by Heidegger in the first section of Being and Time about the dynamics of the existential man understood as being-there (Dasein). Initially is shown the negative character of existence. To do that, we start with the reconstruction of existence concepts and its intentional characteristcs and able to be (Seinkonnen) in Being and Time. In the second part, the analysis of the affective tone of anguish is the starting point to get to the mode of being of man, described carefully by Heidegger (Sorge). We also argue that caution is the only way to be compatible with an entity that in its own way of being is marked by an radical negativity (incomplete). Finally, in the third chapter, we present, in its general features, the possibility compatible with the character of able to be of the being-there: the possibility of death, ontologically understood as being-for-death. In the conclusion, we pointed the greatest interest of Heidegger in his investigation of existential dynamics of the being-there. This interest consist in to visualize, through what Heidegger calls of existential crisis of being-there (provided by the anguish) the genesis point of the ontologies.

Be stars are main-sequence stars and a specific subclass of B type stars with the unique characteristic of showing HI Balmer emission lines in their optical spectra that originates from a circumstellar disk around the star. Over the past 50 years, the Galactic Be star $\\omega$ CMa has exhibited quasi-regular outbursts, every 8 years or so, when the star brightens by about half a magnitude in the V-band. During these outbursts a new disk is formed during the first 3-4 years, and then dissipates in the following 4-6 years. We have access to a rich dataset (including photometry, polarimetry, interferometry and spectroscopy) of $\\omega$ CMa since March 1964 covering several outbursts and quiescence phases. Thus, nature has provided us the perfect experiment to study how Be star disks grow and dissipate. There is an increasing body of evidence that suggests that Be disks are well described by the Viscous Decretion Disk (VDD) model according to which the formation and structure of the disk depend on the kinematic viscosity of the gas. However, most observational tests of the VDD to-date were done for systems that do not display strong temporal variability. We use the rich dataset available for $\\omega$ CMa to perform the first in-depth test of the VDD scenario in a system with strong temporal variability. We use the radiative transfer code HDUST to analyze and interpret the observational dataset. From this analysis we (1) obtain a realistic physical model of the circumstellar environment; (2) measure the viscosity parameter of the gas, both during the formation and dissipation phases of the disk; (3) obtain a reliable estimate of the stellar mass and angular momentum loss rates during outburst. Our simulations offer a good description of the photometric variability, which suggests that the VDD model adequately describes the structural evolution of the disk. Furthermore, our analysis allowed us to determine the viscosity parameter $\\alpha$, as well as the net mass and angular momentum (AM) loss rates. We find that $\\alpha$ is variable, ranging from 0.1 to 1.0, not only from cycle to cycle but also within a given cycle. Additionally, build-up phases have larger values of $\\alpha$ than the dissipation phases. We also find that, contrary to what is generally assumed, during dissipation the outward AM flux is not necessarily zero, meaning that $\\omega$ CMa does not experience a true quiescence but, instead, switches between a high AM loss rate state to a low AM loss rate one during which the disk quickly assumes an overall lower density but never zero. We confront the average AM loss rate with predictions from stellar evolution models for fast-rotating stars, and find that our measurements are smaller by more than one order of magnitude. The model developed using the V-band photometry as a constraint was applied to several other observables. Overall, the results of this multi-technique study were very positive, with a good match for multi-band photometry, polarization, and most spectroscopic characteristics. This is a very relevant result, as it proves that a model that was constructed from constraints only from the very inner part of the disk (the $V$-band light curve), could be extended to the whole disk and to other physical processes. / Estrelas Be são um subtipo específico de estrelas de sequência principal de tipo espectral B. Elas possuem características únicas tais como a presença de linhas de emissão em seu espectro, que se originam de um disco circunstelar. Nos últimos 50 anos, a estrela Be galáctica CMa exibiu erupções quasi-regulares, a cada 8 anos aproximadamente, onde a estrela torna-se mais brilhante na banda V. Nestas erupções um novo disco se forma nos primeiros 3-4 anos e depois dissipa-se nos 4-6 anos seguintes. Temos acesso a uma base de dados rica (incluindo fotometria, polarimetria, interferometria e espectroscopia) de CMa desde março de 1964, que cobre vários ciclos de erupções e quiescências. Assim, a natureza nos proveu um experimento perfeito para estudar como discos de estrelas Be crescem e dissipam-se. Há um corpo de evidências cada vez maior que sugerem que os discos de estrela Be são bem descritos pelo modelo de decréscimo viscoso (VDD), segundo o qual a formação e estrutura do disco depende da viscosidade cinemática do gás. Entretanto, a maioria dos testes conduzidos com o VDD até o momento foram feitos para sistemas que não mostram forte variabilidade temporal. Usamos a rica base de dados de CMa para conduzir o primeiro teste aprofundado do VDD em um sistema fortemente variável. Usamos o código de transporte radiativo HDUST para analisar e interpretar os dados. Desta análise obtemos (1) um modelo fisicamente realista do ambiente circunstelar, (2) a viscosidade do gás, e (3) uma estimativa confiável das taxas de perda de massa e momento angular durante os eventos de formação do disco. Nossas simulações conseguem reproduzir a variabilidade fotométrica muito bem, o que sugere que o modelo VDD descreve corretamente a evolução estrutural do disco. Mostramos que o parâmetro de viscosidade é variável, com valores entre 0.1 e 1. Adicionalmente, as fases de construção do disco têm valores de viscosidade maior. Contrariamente ao que se acredita, mostramos que durante a dissipação a taxa de perda de momento angular não é necessariamente nula, o que implica que CMa não experimenta uma quiescência verdadeira, mas alterna entre uma fase de alta taxa de perda de momento angular (erupção) e uma fase de baixa taxa (quiescência). Confrontamos as taxas de perda de momento angular com as preditas pelos modelos evolutivos de Genebra, e encontramos que nossas taxas são mais que 10 vezes menores que as taxas de previstas pelos modelos. O modelo desenvolvido para reproduzir a curva de luz na banda V foi aplicado a vários outros observáveis. De forma geral, os resultados deste estudo multi-técnica foram muito positivos, com uma boa concordância com a fotometria multi-banda, polarização, e a maioria das características espectrais. Este é um resultado muito relevante, pois prova que um modelo que foi construído apenas a partir de vínculos para a interna do disco (a curva de luz na banda V), pode ser estendido para todo o disco e também outros processos físicos.

Herbig Ae/Be (HAeBe) stars are intermediate mass (2-10 solar mass) pre-main sequence stars with circumstellar disks. Observing planets within these young disks would greatly aid in understanding planet formation processes and timescales particularly around massive stars. So far, only one planet, HD 100546 b, has been confirmed to orbit a HAeBe star. With over 250 HAeBe stars known, and several observed to have disks with structures thought to be related to planet formation, it seems likely that there are as yet undiscovered planetary companions within the circumstellar disks of some of these young stars. Direct detection of a low-luminosity companion near a star requires high contrast imaging, often with the use of a coronagraph, and the subtraction of the central star's point spread function (PSF). Several processing algorithms have been developed in recent years to improve PSF subtraction and enhance the signal-to-noise of sources close to the star. However, many HAeBe stars were observed via direct imaging before these algorithms came out. We used the PSF subtraction program PynPoint to reprocess archival images of HAeBe stars from the Advanced Camera for Surveys on the Hubble Space Telescope to increase the likelihood of detecting a planet in their disks. We believe we have recovered the known planet around HD 100546 and possibly its candidate second companion. We also detect new candidate sources in the vicinities of HD 141569 and HD 163296. Further observations are needed to confirm the reality of these detections and also establish their association with the host stars.

L’attrait récent des autorités françaises pour le développement de la médecine génétique a attiré notre attention. Si aujourd’hui elle tend à gagner une place centrale dans l’offre de santé française, notamment, par l’adoption du projet « France génomique 2025 », elle engendre des questions éthiques et juridiques complexes. L’intérêt pour la parentèle de connaître le risque génétique du patient afin de bénéficier d’une prise en charge précoce du risque héréditaire familial a soulevé de larges débats. Pour cause, la préservation de la santé de ces tiers à la relation médicale entre de manière inévitable en conflit avec le droit fondamental au secret médical des patients. La France a été un des premiers pays à tenter de répondre à ce problème en apparence insoluble. Par deux lois de bioéthiques de 2004 et 2011, le législateur a créé un régime visant à apporter un équilibre entre ces deux questions. Alors que les parlementaires vont bientôt se réunir afin de réviser une nouvelle fois les lois de bioéthique, nous souhaitons dresser un état des lieux de la conciliation actuelle entre les intérêts des patients et de leurs consanguins. L’objectif de cette analyse sera d’identifier les difficultés rencontrées par les parlementaires nationaux et de proposer des solutions afin de faire avancer le droit français dans sa quête de création d’un juste équilibre entre les droits des patients et des apparentés. Cette étude conjointe des droits français et étrangers nous conduira à proposer la création d’un nouvel outil d’équilibre au service de la santé publique : le dossier médical familial / The recent attraction of the French authorities for the development of the genetic medicine drew our attention. The establishment of the project "France genomic 2025” tends to place the genetic medicine in the center of the medical services. However, it engenders complex ethical and legal questions. The interest of the relatives to be informed in case of a serious risk for their health have raised wide debates. The protection of the health of these third parties in the patient—physician relationship enters in conflict with the patient’s right of confidentiality. French authorities were among the first to try to create a balance between those two interests. The objective of this analysis will be to identify the difficulties met by the parliament and to propose solutions to advance the French law in its research of creation of a just balance between the rights of the patients and the allies. This joint study of the French and foreign rights will lead us to propose the creation of a new tool of balance in the service of the public health