Estratégia do planejamento e otimização de sistemas sem fio, considerando redes interferentes: abordagem baseada em cross-layer

Apesar do aumento significativo do uso de redes locais sem fio (WLAN) nos últimos anos, aspectos de projeto e planejamento de capacidade da rede são ainda sistematicamente negligenciados durante a implementação da rede. Tipicamente um projeto de rede local sem fio é feito e instalado por profissionais de rede. Esses profissionais são extremamente experientes com redes cabeadas, mas são ainda geralmente pouco experientes com redes sem fio. Deste modo, as instalações de redes locais sem fio são desvantajosas pela falta de um modelo de avaliação de desempenho e para determinar a localização do ponto de acesso (PA), além disso, fatores importantes do ambiente não são considerados no projeto. Esses fatores se tornam mais importante quando muitos pontos de acesso (PAs) são instalados para cobrir um único edifício, algumas vezes sem planejamento de freqüência. Falhas como essa podem causar interferência entre células geradas pelo mesmo PA. Por essa razão, a rede não obterá os padrões de qualidade de serviço (QoS) exigidos por cada serviço. O presente trabalho apresenta uma proposta para planejamento de redes sem fio levando em consideração a influência da interferência com o auxílio de inteligência computacional tais como a utilização de redes Bayesianas. Uma extensiva campanha de medição foi feita para avaliar o desempenho de dois pontos de acesso (PAs) sobre um cenário multiusuário, com e sem interferência. Os dados dessa campanha de medição foram usados como entrada das redes Bayesianas e confirmaram a influência da interferência nos parâmetros de QoS. Uma implementação de algoritmo genético foi utilizado permitindo uma abordagem híbrida para planejamento de redes sem fio. Como efeito de comparação para otimizar os parâmetros de QoS, de modo a encontrar a melhor distância do PA ao receptor garantindo as recomendações do International Telecomunication Union (ITU-T), a técnica de otimização por enxame de partículas foi aplicada.

Modelos paramétricos simples e causais para cabos de cobre apropriados para caracterização de enlaces em sistemas G.fast

O G.fast é um novo padrão da União Internacional de Telecomunicações que almeja atingir 1 Gb/s sobre enlaces de cobre curtos, utilizando freqüências de até 212 MHz. Essa nova tecnologia requer modelos paramétricos precisos de cabo para fins de projeto, simulação e testes de avaliação de desempenho. A maioria dos modelos de cabo de cobre foram desenvolvidos focando o espectro VDSL - isto é, freqüências de até 30 MHz - e adotam suposições que são violadas quando a faixa de freqüência é estendida para freqüências G.fast. Esta tese apresenta novos modelos de cabo simples e causais capazes de caracterizar com precisão enlaces de cobre compostos por segmentos individuais ou múltiplos, tanto no domínio do tempo quanto no domínio da freqüência. Resultados utilizando as topologias de referência do padrão G.fast mostram que, além de serem precisos, os novos modelos são atrativos devido ao baixo custo computacional e fórmulas fechadas para ajuste de seus parâmetros junto a dados medidos.

A organização internacional dos trabalhadores metalúrgicos na Mercedes-Benz: perspectivas de contra-hegemonia local-global

Pós-graduação em Relações Internacionais (UNESP - UNICAMP - PUC-SP) - FFC

Prospect on intergalactic magnetic field measurements with gamma-ray instruments

Observing high-energy gamma-rays from Active Galactic Nuclei (AGN) offers a unique potential to probe extremely tiny values of the intergalactic magnetic field (IGMF), a long standing question of astrophysics, astropa rticle physics and cosmology. Very high energy (VHE) photons from blazars propagating along the line of sight interact with the extragalactic background light (EBL) and produce e + e − pairs. Through inverse-Compton interaction, mainly on the cosmic microwave background (CMB), these pairs generate secondary GeV-TeV compo- nents accompanying the primary VHE signal. Such secondary components would be detected in the gamma-ray range as delayed “pair echos” for very weak IGMF ( B< 10 − 16 G ), while they should result in a spatially extended ga mma-ray emission around the source for higher IGMF values ( B> 10 − 16 G ). Coordinated observations with space (i.e. Fermi) and ground- based gamma-ray instruments, such as the pre sent Cherenkov experiments H.E.S.S., MAGIC and VERITAS, the future Cherenkov Telescope Array (CTA) Observatory, and the wide-field detectors such as HAWC and LHAASO, should allow to analyze and finally detect such echos, extended emission or pair halos, and to further characterize the IGMF.

The star formation rate in the inner Milky Way Galaxy

The present star formation rate (SFR) in the inner Galaxy is puzzling for the chemical evolution models (CEM). No static CEM is able to reproduce the peak of the SFR in the 4 kpc ring. The main reason is probably a shortage of gas, which could be due to the dynamical effects produced by the galactic bar, not considered by these models. We developed a CEM that includes radial gas flows in order to mimic the effects of the galactic bar in the first 5 kpc of the galactic disk. In this model, the star formation (SF) is a two-step process: first, the diffuse gas forms molecular clouds. Then, stars form from cloud-cloud collisions or by the interaction between massive stars and the molecular gas. The former is called spontaneous and the latter induced SF. The mass in the different phases of each region changes by the processes associated with the stellar formation and death by: the SF due to spontaneous fragmentation of gas in the halo; formation of gas clouds in the disk from the diffuse gas; induced SF in the disk due to the interaction between massive stars and gas clouds; and finally, the restitution of the diffuse gas associated to these process of cloud and star formation. In the halo, the star formation rate for the diffuse gas follows a Schmidt law with a power n = 1.5. In the disk, the stars form in two steps: first, molecular clouds are formed from the diffuse gas also following a Schmidt law with n=1.5 and a proportionality factor. Including a specific pattern of radial gas flows, the CEM is able to reproduce with success the peak in the SFR at 4 kpc (fig. 1).

Magnetic color-flavor-locked stars

Using the solutions of the gap equations of the magnetic-color-flavor-locked (MCFL) phase of paired quark matter in a magnetic field, and taking into consideration the separation between the longitudinal and transverse pressures due to the field-induced breaking of the spatial rotational symmetry, the equation of state (EoS) of the MCFL phase is self-consistently determined. Implications for stellar models of magnetized (self-bound) strange stars and hybrid (MCFL core) stars are discussed.

Trigonometric parallaxes in the TW Hydrae Association

We have conducted a program of trigonometric distance measurements to 13 members of the TW Hydrae Association (TWA), which will enable us (through back-tracking methods) to derive a convincing estimate of the age of the association, independent of stellar evolutionary models. With age, distance, and luminosity known for an ensemble of TWA stars and brown dwarfs, models of early stellar evolution (which are still uncertain for young ages and substellar masses) will then be constrained by observations over a wide range of masses (0.025 to 0.7 M⊙).

Kinematic distances of pre-main-sequence stars in the Lupus star-forming region

To reliably determine the main physical parameters (masses and ages) of young stars, we must know their distances. While the average distance to nearby star-forming regions (<300 pc) is often known, the distances to individual stars are usually unknown. Individual distances to members of young moving groups can be derived from their radial velocities and proper motions using the convergent-point strategy. We investigate the kinematic properties of the Lupus moving group with the primary objective of deriving individual distances to all group members.

Planetary nebulae and determination of the bulge-disk boundary

In this paper, a sample of planetary nebulae in the Galaxy's inner-disk and bulge is used to find the galactocentric distance that optimally separates these two populations in terms of their abundances. Statistical distance scales were used to investigate the distribution of abundances across the disk–bulge interface, while a Kolmogorov–Smirnov test was used to find the distance at which the chemical properties of these regions separate optimally. The statistical analysis indicates that, on average, the inner population is characterized by lower abundances than the outer component. Additionally, for the α-element abundances, the inner population does not follow the disk's radial gradient toward the Galactic Center. Based on our results, we suggest a bulge–disk interface at 1.5 kpc, marking the transition between the bulge and the inner disk of the Galaxy as defined by the intermediate-mass population.

Mobile goes global: The effect of cell phones on economic growth and development

This study investigates the effect of cell phones on economic development and growth by performing an econometric analysis using data from the International Telecommunications Union and the Penn World Table. It discusses the various ways cell phones can make markets more efficient and how the diffusion of information andknowledge plays into development. Several approaches (OLS, Fixed Effects, 2SLS) were used to test over 20 econometric models. Overall, the mobile cellular subscriptions rate was found to have a positive and significant impact on countries’ level of real per capitaGDP and GDP growth rate. Furthermore, the study provides policy implications for the use of technology to promote global growth.

Global Change and the World's Mountain. Where are we coming from, and where are we going to?

The history of mountain research is most fascinating. Three names for 3 centuries may give an idea of the growing knowledge about the world's mountains: Horace Bénédict de Saussure, who climbed and studied the Mont Blanc in 1787; Alexander von Humboldt, ever investigating the environment during his attempt to ascend the Chimborazo in 1802; and Carl Troll, who founded the International Geographical Union's Commission on High-altitude Geoecology in 1968. Awareness of the growing impact of human activities on the environment led to scientific and political initiatives at the global level, beginning in the 1970s. The Perth conference in 2010 has offered an opportunity to both look back on these developments and explore the future of the world's mountains in a time of rapidly growing “global change” problems and processes.