Astrochemistry

In the last 40 years a wide range of molecules, including neutrals, cations and anions, containing up to 13 atoms—in addition to detections of C₆₀ and C₇₀ — have been found in the harsh environment of the interstellar medium. The exquisite sensitivity and very high spectral and, more recently, spatial resolution, of modern telescopes has enabled the physics of star formation to be probed through rotational line emission. In this article, I review the basic properties of interstellar clouds and the processes that initiate the chemistry and generate chemical complexity, particularly in regions of star and planet formation. Our understanding of astrochemistry has evolved over the years. Before 1990, the general consensus was that molecules were formed in binary, gas-phase, or volume, reactions, most importantly ion-neutral reactions despite the very low ionization in clouds. Since then, observations have indicated unambiguously that there is also a contribution from surface processes, particularly on the icy mantles that form around refractory grain cores in cold, dense gas. The balance between these two processes depends on particular physical conditions and can vary during the life cycle of a particular volume of interstellar cloud.The complex chemistry that occurs in space is driven mostly through interaction of thegas with cosmic ray protons, a source of ionization that enables a rich ion-neutral chemistry. In addition, I show that the interaction between the gas and the dust in cold, dense regionsalso leads to additional chemical complexity through reactions that take place in ices at onlya few tens of degrees above absolute zero. Although densities are low compared to those in terrestrial environments, the extremely long life times of interstellar clouds and their enormous sizes, enable complex molecules to be synthesised and detected. I show that in some instances, particularly in reactions involving deuterium, the rotational populations of reactants, together with spin-selection rules, can determine the detailed abundances. Although the review is mainly focused on regions associated with star formation, I also consider chemistry in other interesting astronomical regions — in the early Universe and in the envelopes formed by mass loss during the final stages of stellar evolution.

Developed turbulence and nonlinear amplification of magnetic fields in laboratory and astrophysical plasmas

The visible matter in the universe is turbulent and magnetized. Turbulence in galaxy clusters is produced by mergers and by jets of the central galaxies and believed responsible for the amplification of magnetic fields. We report on experiments looking at the collision of two laser-produced plasma clouds, mimicking, in the laboratory, a cluster merger event. By measuring the spectrum of the density fluctuations, we infer developed, Kolmogorov-like turbulence. From spectral line broadening, we estimate a level of turbulence consistent with turbulent heating balancing radiative cooling, as it likely does in galaxy clusters. We show that the magnetic field is amplified by turbulent motions, reaching a nonlinear regime that is a precursor to turbulent dynamo. Thus, our experiment provides a promising platform for understanding the structure of turbulence and the amplification of magnetic fields in the universe.

Thin-shell instability in collisionless plasma

Thin-shell instability is one process which can generate entangled structures in astrophysical plasma on collisional (fluid) scales. It is driven by a spatially varying imbalance between the ram pressure of the inflowing upstream plasma and the downstream's thermal pressure at a nonplanar shock. Here we show by means of a particle-in-cell simulation that an analog process can destabilize a thin shell formed by two interpenetrating, unmagnetized, and collisionless plasma clouds. The amplitude of the shell's spatial modulation grows and saturates after about ten inverse proton plasma frequencies, when the shell consists of connected piecewise linear patches.

Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud

The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H II regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature.

Maxwell perturbations on asymptotically Anti-de-Sitter spacetimes: generic boundary conditions and a new branch of quasinormal modes

Perturbations of asymptotically Anti-de-Sitter (AdS) spacetimes are often considered by imposing field vanishing boundary conditions (BCs) at the AdS boundary. Such BCs, of Dirichlet-type, imply a vanishing energy flux at the boundary, but the converse is, generically, not true. Regarding AdS as a gravitational box, we consider vanishing energy flux (VEF) BCs as a more fundamental physical requirement and we show that these BCs can lead to a new branch of modes. As a concrete example, we consider Maxwell perturbations on Kerr-AdS black holes in the Teukolsky formalism, but our formulation applies also for other spin fields. Imposing VEF BCs, we find a set of two Robin BCs, even for Schwarzschild-AdS black holes. The Robin BCs on the Teukolsky variables can be used to study quasinormal modes, superradiant instabilities and vector clouds. As a first application, we consider here the quasinormal modes of Schwarzschild-AdS black holes. We find that one of the Robin BCs yields the quasinormal spectrum reported in the literature, while the other one unveils a new branch for the quasinormal spectrum.

201186

How is it possible that civilization has a global understanding of the abstraction of the human form? At a subconscious level as humans we have the ability to find the form of the body in the most minimal of shapes, objects, landscape and even natural phenomena such as clouds, it is an ability inherent in human nature. This deep-rooted facility to recognise the human form at various levels of abstraction is also developed further by our life experiences, environment and total education; specifically in the fine and applied arts. For this research I have focused on the change between realistic representations of the human form to complete abstraction. I have broken it down to its most basic elements to explore at what point our visual language allows us to recognise and define a shape or object as being influenced by, or connected to, the human form. I have concentrated on extending my own visual language relating to the human form within my own practice. A series of practical research projects has been undertaken and has been supported by a new series of investigative works, drawings and written evidence of the ways in which the figure can be represented, documenting the process via the thesis and final works. As part of my research, I have investigated the way artists working with clay have abstracted the human form focusing in particular on work from the 1950s to the present day using clay, drawing and installation. I have looked at how, over this period, artists have developed their own visual signifiers of the human form within their abstract/representational creations. The aim of this research will be falls into two parts: • To investigate how far one can push the human form in clay before it moves into abstraction • To locate the vanishing point where viewers still identify the human within ceramic abstract sculpture

Guest reputation indexes to analyze hotel’s online reputation using data extracted from OTAs

Nowadays many travelers use online travel agency (OTAs) to book flights, hotel rooms, rent-a-cars, cruises or entire vacation packages. Usually OTAs allow their users to give scores and to write reviews about what was used. Each OTA defines the terms and conditions for guest rating or review score and hoteliers are giving increasing importance to the scores and reviews their guests do in OTAs. This paper proposes two guest reputation index to help hoteliers to monitorize their presence in OTAs. The Aggregated Guest Reputation Index (AGRI), which shows the positioning of a hotel in different OTAs and it is calculated from the scores obtained by the hotels in those OTAs. Another one, the Semantic Guest Reputation Index (SGRI), which incorporates the social reputation of a hotel and that can be visualized through the development of word clouds or tag clouds. Examples of usage of these indexes are given with data extracted from 5-stars hotels in the Algarve, south region of Portugal, that are available on Booking and Expedia.

Caracterização e modelação de fissuras em edifícios utilizando 3D laser scanning, com vista à sua reabilitação

Trabalho Final de Mestrado para obtenção do grau de Mestre em Engenharia Civil

Cloud computing sobre a plataforma Windows Azure

A utilização massiva da internet e dos serviços que oferece por parte do utilizador final potencia a evolução dos mesmos, motivando as empresas a apostarem no desenvolvimento deste tipo de soluções. Requisitos como o poder de computação, flexibilidade e escalabilidade tornam-se cada vez mais indissociáveis do desenvolvimento aplicacional, o que leva ao surgimento de paradigmas como o de Cloud Computing. É neste âmbito que surge o presente trabalho. Com o objetivo de estudar o paradigma de Cloud Computing inicia-se um estudo sobre esta temática, onde é detalhado o seu conceito, a sua evolução histórica e comparados os diferentes tipos de implementações que suporta. O estudo detalha posteriormente a plataforma Azure, sendo analisada a sua topologia e arquitetura, detalhando-se os seus componentes e a forma como esta mitiga alguns dos problemas mencionados. Com o conhecimento teórico é desenvolvido um protótipo prático sobre esta plataforma, em que se exploram algumas das particularidades da topologia e se interage com as principais redes sociais. O estudo culmina com uma análise sobre os benefícios e desvantagens do Azure e através de um levantamento das necessidades da empresa, determinam-se as oportunidades que a utilização da plataforma poderá proporcionar.

Observatório de favelas (Rio de Janeiro): a comunicação institucional e a comunicação para o desenvolvimento

Relatório de estágio apresentado à Escola Superior de Comunicação Social como parte dos requisitos para obtenção de grau de mestre em Gestão Estratégica das Relações Públicas.

Ownserver: sistema doméstico de prestação de serviços cloud

Neste trabalho foi considerada a possibilidade de incorporar serviços remotos, normalmente associados a serviços web e cloud computing, numa solução local que centralizasse os vários serviços num único sistema e permitisse aos seus utilizadores consumir e configurar os mesmos, quer a partir da rede local, quer remotamente a partir da Internet. Desta forma seria possível conciliar o acesso a partir de qualquer local com internet, característico nas clouds, com a simplicidade de concentrar num só sistema vários serviços que são por norma oferecidos por entidades distintas e ainda permitir aos seus utilizadores o controlo e configuração sobre os mesmos. De forma a validar que este conceito é viável, prático e funcional, foram implementadas duas componentes. Um cliente que corre nos dispositivos dos utilizadores e que proporciona a interface para consumir os serviços disponíveis e um servidor que irá conter e prestar esses serviços aos clientes. Estes serviços incluem lista de contactos, mensagens instantâneas, salas de conversação, transferência de ficheiros, chamadas e conferências de voz e vídeo, pastas remotas, pastas sincronizadas, backups, pastas partilhadas, VoD (Video-on Demand) e AoD (Audio-on Demand). Para o desenvolvimento do cliente e do servidor foi utilizada a framework Qt que recorre à linguagem de programação C++ e ao conjunto de bibliotecas que possui, para o desenvolvimento de aplicações multiplataforma. Para as comunicações entre clientes e servidor, foi utilizado o protocolo XMPP (Extensible Messaging and Presence Protocol), pela forma da biblioteca qxmpp e do servidor XMPP ejabberd. Pelo facto de conter um conjunto de centenas de extensões atualmente ativas que auferem funcionalidades como salas de conversação, transferências de ficheiros e até estabelecer sessões multimédia, graças à sua flexibilidade permitiu ainda a criação de extensões personalizada necessárias para algumas funcionalidades que se pretendeu implementar. Foi ainda utilizado no servidor a framework ffmpeg para suportar algumas funcionalidades multimédia. Após a implementação do cliente para Windows e Linux, e de implementar o servidor em Linux foi realizado um conjunto de testes funcionais para perceber se as funcionalidades e seus mecanismos funcionam corretamente. No caso onde a análise da performance e do consumo de recursos era importante, foram realizados testes de performance e testes de carga.

Building 3D City Models: Testing and Comparing Laser Scanning and Low-Cost UAV Data Using FOSS Technologies

Contém resumo

View of Falls from Steel Bridge, Niagara, U.S.A.

The description of the image reads "(4)-8972-General view of Falls from new steel bridge - Maid of the Mist at landing - Niagara, U.S.A." The reverse of the image includes the description, "We are standing on the new steel bridge over Niagara River, 190 feet above the water and looking a little west of south, up the river towards Lake Erie. The high cliff at the extreme left, on the American side, is Prospect Point, where a crowd is gathered at this moment to view the Falls that we see just beyond Prospect Point. That dark, tree-covered mass of rock beyond is Goat Island; and just this side of Goat Island we see a bit of its precipice has been cut off separate from the rest by the powerful current of the waters - the smaller portion is Luna Island, and the Luna Falls go pouring down between the two islands. The face of the precipice curves inward beneath the Luna Falls leaving behind the 160 foot sheet of water the unearthly hollow known as the Cave of the Winds. Beyond Goat Island we see the gigantic curve of the Horseshoe Falls, 3,010 feet long and 158 feet high, reaching around through the clouds of spray to the farther Canadian shore. (The boundary line between British and American territory is in mid-stream.) It has been estimated that every minute 375,000 tons of water pour over these Horseshoe Falls, and they are wearing away the cliffs, moving back up the stream at the rate of 2.4 feet per year. It was probably only about a thousand years ago that they took their plunge just about where we stand now. Down there below us, at the wharf is the Maid of the Mist at the American landing taking on passengers who have come down the steep bank by the inclined railway. Its course takes it through those clouds of spray almost to the very foot of both Falls, - waters falling from 167 feet overhead, and water surging at least as many feet deep under the staunch little vessel. See special 'keyed' maps of Niagara pub. by Underwood and Underwood, also the Niagara Book by Mark Twain, W.D. Howells and others."

Analyse multi-échelle des champs magnétiques dans des nuages moléculaires à structures filmentaires

Associée à d'autres techniques observationnelles, la polarimétrie dans le visible ou dans le proche infrarouge permet d'étudier la morphologie des champs magnétiques à la périphérie de nombreuses régions de formation stellaire. A l'intérieur des nuages molécualires la morphologie des champs est connue par polarimétrie submillimétrique, mais rarement pour les mêmes régions. Habituellement, il manque une échelle spatiale intermédiaire pour pouvoir comparer correctement la morphologie du champ magnétique galactique avec celle située à l'intérieur des nuages moléculaires. -- Cette thèse propose les moyens nécessaires pour réaliser ce type d'analyse multi-échelle afin de mieux comprendre le rôle que peuvent jouer les champs magnétiques dans les processus de formation stellaire. La première analyse traite de la région GF 9. Vient ensuite une étude de la morphologie du champ magnétique dans les filaments OMC-2 et OMC-3 suivie d'une analyse multi-échelle dans le complexe de nuages moléculaires Orion A dont OMC-2 et OMC-3 font partie. -- La synthèse des résultats couvrant GF 9 et Orion A est la suivante. Les approches statistiques employées montrent qu'aux grandes échelles spatiales la morphologie des champs magnétiques est poloïdale dans la région GF 9, et probablement hélicoïdale dans la région Orion A. A l'échelle spatiale des enveloppes des nuages moléculaires, les champs magnétiques apparaissent alignés avec les champs situés à leur périphérie. A l'échelle spatiale des coeurs, le champ magnétique poloïdal environnant la région GF 9 est apparemment entraîné par le coeur en rotation, et la diffusion ambipolaire n'y semble pas effective actuellement. Dans Orion A, la morphologie des champs est difficilement détectable dans les sites actifs de formation d'OMC-2, ou bien très fortement contrainte par les effets de la gravité dans OMC-1. Des effets probables de la turbulence ne seont détectés dans aucune des régions observées. -- Les analyses multi-échelles suggèrent donc qu'indépendamment du stade évolutif et de la gamme de masse des régions de formation stellaires, le champ magnétique galactique subit des modifications de sa morphologie aux échelles spatiales comparables à celles des coeurs protostellaires, de la même façon que les propriétés structurelles des nuages moléculaires suivent des lois d'autosimilarité jusqu'à des échelles comparables à celles des coeurs.