Submitted by Irvana Coutinho (irvana@ufpa.br) on 2012-01-09T14:24:14Z No. of bitstreams: 2 Dissertacao_EvagreloSilvaAnaliseImplementacaoPlanos.pdf: 5866653 bytes, checksum: 94c625b6f4ddfcfed946504987989be9 (MD5) license_rdf: 23892 bytes, checksum: afd5dad10b1d1e6dc10c8c5d25222c7a (MD5) / Approved for entry into archive by Irvana Coutinho(irvana@ufpa.br) on 2012-01-09T14:24:57Z (GMT) No. of bitstreams: 2 Dissertacao_EvagreloSilvaAnaliseImplementacaoPlanos.pdf: 5866653 bytes, checksum: 94c625b6f4ddfcfed946504987989be9 (MD5) license_rdf: 23892 bytes, checksum: afd5dad10b1d1e6dc10c8c5d25222c7a (MD5) / Made available in DSpace on 2012-01-09T14:24:57Z (GMT). No. of bitstreams: 2 Dissertacao_EvagreloSilvaAnaliseImplementacaoPlanos.pdf: 5866653 bytes, checksum: 94c625b6f4ddfcfed946504987989be9 (MD5) license_rdf: 23892 bytes, checksum: afd5dad10b1d1e6dc10c8c5d25222c7a (MD5) Previous issue date: 2005 / CNPq - Conselho Nacional de Desenvolvimento Científico e Tecnológico / O estudo teve por objetivo verificar a coerência dos Planos de Recuperação de Áreas Degradadas (PRADs) pela Mineração Novo Astro - MNA no Distrito de Lourenço, Município de Calçoene (AP), a partir do conhecimento do contexto em que se estabeleceram e foram decididas as medidas de recuperação, e quais os atores que influenciaram neste processo de decisão. Foram realizadas entrevistas com membros da população e com representantes da MNA, da Ampla Engenharia (empresa responsável pela recuperação do ambiente degradado), da Cooperativa de Garimpeiros de Lourenço - COOGAL, da Secretaria Especial de Meio Ambiente do Amapá - SEMA, do Departamento Nacional da Produção Mineral - DNPM, do Ministério Público Federal, do governo do Estado, e da prefeitura Municipal de Calçoene. Estes atores influenciaram de forma decisiva para os resultados agora observados no local. A pesquisa envolveu o estudo sobre as medidas de recuperação mais eficazes em voga, a história dos acontecimentos em Lourenço e o contexto socioeconômico, para que fossem compreendidas as possibilidades de êxito das medidas escolhidas para o local. A partir destes dados foi feita a análise da eficácia destes PRADs e tecidas alternativas e direcionamentos futuros para o local, baseados nas características sociais e ambientais de Lourenço. O primeiro PRAD, finalizado em 1995, terminou por apresentar resultados pouco consistentes, de tal forma que o local no qual este foi executado voltou a ser explorado pelos garimpeiros e continuou a estar em condições degradadas. A MNA, por não ter legalizado sua situação, foi responsabilizada pela nova recuperação do local em 2002. O segundo PRAD, parcialmente implementado em 2003, possuiu baixa eficácia, com a morte de mais de 70% das espécies vegetais utilizadas em algumas áreas. A falta de conhecimentos mais profundos, por parte das empresas de mineração e de recuperação ambiental, sobre as características do meio ambiente e do contexto socioeconômico local parecem ter contribuído para os resultados negativos da implementação dos PRADs. Uma alternativa seria buscar a participação da população local nos projetos e políticas criados para a região, como forma de criar soluções que contemplem as características locais e os desejos da população. / This work aims at verifying the existence of Degraded Area Recuperation Plans (DARP’s) made by Mineração Novo Astro – MNA (Novo Astro mining company), in the district of Lourenço, Municipality of Calçoene, State of Amapá, Brazil, based on the knowledge of recuperation measures created and decided within a framework, and to identify who were the actors that influenced this decision making process. Interviews were conducted with members of the local population, and representatives of the following organizations: MNA, Ampla Engenharia (engineering company hired to recuperate the degraded environment), the Lourenço Mining Cooperative (COOGAL), the Amapá State Special Agency for the Environment (SEMA), the National Department of Mineral Production (DNPM), the Federal Public Attorney’s Office, State Government, and Calçoene City Hall. These actors had a decisive influence on the local results seen today. The research included studies on existent recuperation measures, historical facts occurred in Lourenço, and the social and economic context in order to understand the successful measures chosen for that place. From such data, an analysis of the DARP efficiency was conducted, and alternatives and future guidelines were suggested, based on the social and environmental features of Lourenço. The first DARP was concluded in 1995 with pour results, as the place where it was carried out was again explored by miners and remained in a degraded condition. In 2002, MNA was held in charge of the new recuperation, due to its previous failure in complying with legal requirements. The second DARP, which was partially implemented in 2003, has not been very effective, since more than 70% of the species used in some areas have perished. The negative result of both DARP’s may result from the lack of a deeper knowledge on the part of the mining companies and environmental recuperation companies, about the local environmental and socioeconomic framework. An alternative would be to try to gather local people participation on the projects and policies created for the area, in order to come up with adequate solutions for the local population characteristics and desires.

Diagnosing the temperatures and densities of plasmas is critical to the understanding of a wide variety of phenomena. Everything from equations of state for warm dense matter (WDM) found in Jovian planets and inertial confinement fusion (ICF) to turbulent and dissipative processes in laser-produced plasmas, rely on accurate and precise measurements of temperature and density. This work presents improvements on two distinct techniques for measuring temperatures and densities in plasmas: x-ray Thomson scattering (XRTS), and Langmuir probes (LPs). At the OMEGA laser facility, experiments on warm dense matter were performed by firing lasers at an ablator foil and driving a planar shock into cryogenically cooled liquid deuterium. XRTS in the collective scattering regime was implemented to probe the matter, measuring densities of n_e ~ 4.3 x 10²³ cm^-3, temperatures of T_e ~ 12 eV and ionizations of Z ~ 1.0. Through an extension to XRTS theory for inhomogeneous systems, it was possible to extract an additional parameter, the length scale of the shock, whose value of ? ~ 1.33 nm was consistent with the predicted mean free path, and therefore the thickness of the shock. A unique triple Langmuir probe prototype was designed and tested at the Gregori group's lab at the University of Oxford. This probe was designed for a high temporal resolution of ~ 200 MHz for probing laser-produced shocks. The probes were used to measure the shock formed from ablating carbon rods in an argon gas fill. The probe yielded plasma parameters of n_e ~ 1.0 x 10¹⁷ cm^-3 , and T^e ~ 1.5 eV, consistent with measurements from interferometry and emission spectroscopy.

Submitted by Daniella Sodre (daniella.sodre@ufpe.br) on 2015-03-11T13:53:35Z No. of bitstreams: 2 Dissertaçao Joao Ferreira da Silva Jr.pdf: 2184320 bytes, checksum: fb503909f5b1d57d923852e5dafce5b6 (MD5) license_rdf: 1232 bytes, checksum: 66e71c371cc565284e70f40736c94386 (MD5) / Approved for entry into archive by Daniella Sodre (daniella.sodre@ufpe.br) on 2015-03-13T12:59:47Z (GMT) No. of bitstreams: 2 Dissertaçao Joao Ferreira da Silva Jr.pdf: 2184320 bytes, checksum: fb503909f5b1d57d923852e5dafce5b6 (MD5) license_rdf: 1232 bytes, checksum: 66e71c371cc565284e70f40736c94386 (MD5) / Made available in DSpace on 2015-03-13T12:59:47Z (GMT). No. of bitstreams: 2 Dissertaçao Joao Ferreira da Silva Jr.pdf: 2184320 bytes, checksum: fb503909f5b1d57d923852e5dafce5b6 (MD5) license_rdf: 1232 bytes, checksum: 66e71c371cc565284e70f40736c94386 (MD5) Previous issue date: 2013-08-28 / Os avanços tecnológicos acontecem por intermédio de pesquisas e estudos, inclusive com a criação de novos paradigmas, tais como a computação em nuvem, comércio eletrônico e redes sociais. Em alguns casos, grandes centros de dados são utilizados para suportar esses paradigmas. Com isso, estes grandes centros de dados tornaram-se elementos críticos no desenvolvimento de tarefas diárias, o que sugere que, a cada dia, utilizamos mais seus recursos, aumentando a demanda e, consequentemente, o consumo elétrico. Hodiernamente, o consumo de energia é uma questão de interesse comum. Pesquisas demonstram que, como consequência da constante evolução e expansão da tecnologia da informação, os centros de dados e as nuvens (cloud computing) são grandes consumidores de energia elétrica. Com esse alto consumo, destacam-se as questões de sustentabilidade e custo. Neste contexto, a presente dissertação propõe um algoritmo de distribuição de carga elétrica (ADCE) para otimizar a distribuição de energia em infraestruturas elétricas de centros de dados e nuvens privadas. O ADCE é suportado pelo ambiente denominado Mercury, que é capaz de realizar uma avaliação integrada das métricas de confiabilidade, custo e sustentabilidade. O ADCE otimiza, mais especificamente, a distribuição da corrente elétrica na modelagem de fluxo de energia (EFM - Energy Flow Model). A modelagem em EFM é responsável por estimar as questões de sustentabilidade e de custo das infraestruturas elétricas de centros de dados e nuvens, respeitando as restrições de capacidade de energia que cada dispositivo é capaz de fornecer (considerando o sistema elétrico) ou extrair (considerando o sistema de refrigeração). Ademais, dois estudos de caso são apresentados, onde são analisadas sete infraestruturas elétricas de um centro de dados e seis de uma nuvem privada. Para os centros de dados foi alcançada uma redução no consumo de energia de até 15,5% e a métrica utilizada para avaliar a redução do impacto ambiental (exergia) foi reduzida em mais da metade de seu valor. No que concerne ao estudo das nuvens privadas a redução do consumo de energia foi de até 9,7% e da exergia de para quase um terço de seu valor inicial. Os resultados obtidos foram significativos, uma vez que as preocupações ambientais ganham destaque com o passar dos anos e os recursos financeiros das empresas são finitos e muito valiosos.

<p>     </p> <p>This article-based dissertation provides a review of the broad subject of Neutron Star- their emission properties, plasmoids ejection events, and their proposed physical mechanisms. The primary purpose of this dissertation is to provide an extensive description of the research projects I undertook during my tenure as a Graduate Research Assistant, under the guidance of my advisor Prof. Maxim Lyutikov. </p> <p><br></p> <p>Chapter 1 provides a broad overview of the Neutron stars, their classification, proposed emission models, and a summary of magnetars and associated observed phenomena. </p> <p><br></p> <p>In Chapter 2, I present a version of the research article published in the <em>Monthly Notices of the Royal Astronomical Society</em>. The work is titled "Rotating Neutron Stars Without Light Cylinders" and discusses twisted and differentially rotating neutron star magnetospheres that do not have a light cylinder, generate no wind, and thus do not spin down. The magnetosphere of such neutron stars is composed of embedded differentially rotating flux surfaces, with the angular velocity decreasing as Ω ∼ 1/r. It was found, both analytically and using numerical simulations, that for spin parameters larger than some critical value, the light cylinder appears, the magnetosphere opens up, and the wind is generated. </p> <p>In Chapter 3, I present a version of the research article published in <em>The Astrophysical Journal</em>. The work is titled "Relativistic Magnetic Explosions" and was undertaken under the supervision of Dr. Maxim Barkov, in collaboration with Dr. Konstantinos N. Gourgou- liatos and Dr. Lyutikov2 Barkov. It discusses the dynamics of magnetically driven explosive astrophysical events, like magnetar bursts and flares. We model a relativistic expansion of highly magnetized and highly magnetically over-pressurized clouds. We observe that the corresponding dynamics are qualitatively different from fluid explosions due to the topological constraint of the conservation of the magnetic flux. Using analytical, relativistic MHD as well as force-free calculations, we find that the creation of a relativistically expanding, causally disconnected flow obeys a threshold condition: it requires sufficiently high initial over-pressure and sufficiently quick decrease of the pressure in the external medium (the pre-explosion wind). In the subcritical case, the magnetic cloud just puffs up" and quietly expands with the pre-flare wind. We also find a compact analytical solution to the Prendergast problem - the expansion of force-free plasma into the vacuum. </p> <p><br></p> <p>Chapter 4 is the extension of the work in Chapter 3 and focuses on the dynamics of relativistic Coronal Mass Ejections (CMEs), from launching by shearing of foot-points (either slowly or suddenly), to propagation in the preceding magnetar wind. The work has been accepted to be published in <em>Monthly Notices of the Royal Astronomical Society</em>. For slow shear, we find that most of the energy injected into the CME is first spent on the work done on breaking through the over-laying magnetic field. At later stages, sufficiently powerful CMEs may lead to the detonation of a CME and opening of the magnetosphere beyond some equipartition radius req, where the decreasing energy of the CME becomes larger than the decreasing external magnetospheric energy. Post-CME magnetosphere relaxes via the formation of a plasmoid-mediated current sheet, initially at req, and slowly reaching the light cylinder. Both the location of the foot-point shear and the global magnetospheric configuration affect the frequent/weak versus rare/powerful CME dichotomy - to produce powerful flares the slow shear should be limited to field lines that close in near the star.  After the creation of a topologically disconnected flux tube, the tube quickly (at ∼ the light cylinder) comes into force-balance with the preceding wind and is passively advected/frozen in the wind afterward. </p> <p>For fast shear case, the shearing of foot-points leads to the generation of Alfvén wave and the pressure of such Alfvén leads to the opening of the magnetosphere. At distances much larger than the light cylinder, the resulting shear Alfvén waves propagate through the wind non-dissipatively. </p> <p><br></p> <p>In Chapter 5, I switch gears and study the optical polarization of Crab pulsar. I start by deriving a general relation for the polarization direction of the electric dipole-type radiation produced by a particle moving in an arbitrary electromagnetic field. The derived relations are then applied to reproduce optical polarization swings in Crab pulsar assuming a Michel- Bogovalov solution for the current sheet. With this, I was able to reproduce down to intricate details the spin-phase trajectory of the position angle (PA) in the Stokes parameters U-Q plane. This chapter however remains a work in progress. We still don't fully understand the physical mechanism behind the polarization characteristics of the Crab, especially the origin of the point where the inner loop connects with the bigger outer loop. I plan to fully answer these questions before sending our findings for publication. </p> <p><br></p> <p>Chapter 6 summarizes the main results and conclusions of the research projects and mentions the prospects. References are compiled after the appendices so that they are first cited, followed by a CV and a list of publications. </p>

This thesis focuses on the use of narratives and how they connect Astro tourism to sustainability. This research is done from the viewpoint of the narrators and uncovers what narratives they have chosen to present to the visitors, their reasons to include those narratives, what messages they want to convey and how that relates to sustainability. This research was conducted in order to explore how narratives can be used together with Astro tourism to sustainably develop peripheral regions. This thesis uses a qualitative approach with in-depth interviews and inquests. The informants are people who conduct narrated Astro tourism tours in different parts of the world. The findings of this thesis are that in Astro tourism narratives can be used to educate, inspire, shape perceptions, raise awareness and develop environmental consciousness in people. The narratives can take part in the place, value and identity creation processes, can provide a sustainable competitive advantage, can link together the visual aspects and reconnect the visitors to nature and the past. These findings can be used in the broader field of science about narratives and storytelling in the experience-based industry. On a more practical side it is recommended to include narratives that communicate ideas about sustainability that the narrators personally feel passionate about, and they should consider what kind of message they want to convey through them and how that will affect the customer’s experience.

Using a cryogenic linear 22-pole rf ion trap, rate coefficients for H/D exchange reactions of OH− with D2 (1) and OD− with H2 (2) have been measured at temperatures between 11 K and 300 K with normal hydrogen. Below 60 K, we obtained k1 = 5.5 × 10−10 cm3 s−1 for the exoergic reaction (1). Upon increasing the temperature above 60 K, the data decrease with a power law, k1(T) [similar] T−2.7, reaching ≈1 × 10−10 cm3 s−1 at 200 K. This observation is tentatively explained with a decrease of the lifetime of the intermediate complex as well as with the assumption that scrambling of the three hydrogen atoms is restricted by the topology of the potential energy surface. The rate coefficient for the endoergic reaction (2) increases with temperature from 12 K up to 300 K, following the Arrhenius equation, k2 = 7.5 × 10−11 exp(−92 K/T) cm3 s−1 over two orders of magnitude. The fitted activation energy, EA-Exp = 7.9 meV, is in perfect accordance with the endothermicity of 24.0 meV, if one accounts for the thermal population of the rotational states of both reactants. The low mean activation energy in comparison with the enthalpy change in the reaction is mainly due to the rotational energy of 14.7 meV contributed by ortho-H2 (J = 1). Nonetheless, one should not ignore the reactivity of pure para-H2 because, according to our model, it already reaches 43% of that of ortho-H2 at 100 K. / Dieser Beitrag ist aufgrund einer (DFG-geförderten) Allianz- bzw. Nationallizenz frei zugänglich.