Children's sociospatial (re)production of disability within primary school playgrounds

There is a contemporary shift in the institutional context of 'disabled' children's education in the United Kingdom from segregated special to mainstream schools. This change is tied to wider deinstitutionalised or reinstitutionalised geographies of disabled people, fragile globalised educational 'inclusion' agendas, and broader concerns about social cohesiveness. Although coeducating children is expected to transform negative representations of (dis)ability in future society, there are few detailed explorations of how children's everyday sociospatial practices (re)produce or transform dominant representations of (dis)ability. With this in mind, children's contextual and shifting performances of (dis)ability in two case study school playground (recreational) spaces are explored. The findings demonstrate that children with mind-body differences are variously (dis)abled, in comparison with sociospatially shifting norms of ability, which have body, learning, and emotional-social facets. The discussion therefore places an emphasis on the need to incorporate 'intellectual' and 'emotional' differences more fully into geographical studies of disability and identity. The paper has wider resonance for transformative expectations placed on colocating children with a variety of 'axes of difference' (such as gender, 'race, ethnicity, and social class) in schools.

Dynamic portrait of the planetary 2/1 mean-motion resonance - I. Systems with a more massive outer planet

We analyse the global structure of the phase space of the planar planetary 2/1 mean-motion resonance in cases where the outer planet is more massive than its inner companion. Inside the resonant domain, we show the existence of two families of periodic orbits, one associated to the librational motion of resonant angle (sigma-family) and the other related to the circulatory motion of the difference in longitudes of pericentre (Delta pi-family). The well-known apsidal corotation resonances (ACR) appear as intersections between both families. A complex web of secondary resonances is also detected for low eccentricities, whose strengths and positions are dependent on the individual masses and spatial scale of the system. The construction of dynamical maps for various values of the total angular momentum shows the evolution of the families of stable motion with the eccentricities, identifying possible configurations suitable for exoplanetary systems. For low-moderate eccentricities, several different stable modes exist outside the ACR. For larger eccentricities, however, all stable solutions are associated to oscillations around the stationary solutions. Finally, we present a possible link between these stable families and the process of resonance capture, identifying the most probable routes from the secular region to the resonant domain, and discussing how the final resonant configuration may be affected by the extension of the chaotic layer around the resonance region.

Modelling the secular evolution of migrating planet pairs

The subject of this paper is the secular behaviour of a pair of planets evolving under dissipative forces. In particular, we investigate the case when dissipative forces affect the planetary semimajor axes and the planets move inwards/outwards the central star, in a process known as planet migration. To perform this investigation, we introduce fundamental concepts of conservative and dissipative dynamics of the three-body problem. Based on these concepts, we develop a qualitative model of the secular evolution of the migrating planetary pair. Our approach is based on the analysis of the energy and the orbital angular momentum exchange between the two-planet system and an external medium; thus no specific kind of dissipative forces is invoked. We show that, under the assumption that dissipation is weak and slow, the evolutionary routes of the migrating planets are traced by the Mode I and Mode II stationary solutions of the conservative secular problem. The ultimate convergence and the evolution of the system along one of these secular modes of motion are determined uniquely by the condition that the dissipation rate is sufficiently smaller than the proper secular frequency of the system. We show that it is possible to reassemble the starting configurations and the migration history of the systems on the basis of their final states and consequently to constrain the parameters of the physical processes involved.

Dynamic portrait of the planetary 2/1 mean-motion resonance - II. Systems with a more massive inner planet

This paper presents the second part in our study of the global structure of the planar phase space of the planetary three-body problem, when both planets lie in the vicinity of a 2/1 mean-motion resonance. While Paper I was devoted to cases where the outer planet is the more massive body, the present work is devoted to the cases where the more massive body is the inner planet. As before, outside the well-known Apsidal Corotation Resonances (ACR), the phase space shows a complex picture marked by the presence of several distinct regimes of resonant and non-resonant motion, crossed by families of periodic orbits and separated by chaotic zones. When the chosen values of the integrals of motion lead to symmetric ACR, the global dynamics are generally similar to the structure presented in Paper I. However, for asymmetric ACR the resonant phase space is strikingly different and shows a galore of distinct dynamical states. This structure is shown with the help of dynamical maps constructed on two different representative planes, one centred on the unstable symmetric ACR and the other on the stable asymmetric equilibrium solution. Although the study described in the work may be applied to any mass ratio, we present a detailed analysis for mass values similar to the Jupiter-Saturn case. Results give a global view of the different dynamical states available to resonant planets with these characteristics. Some of these dynamical paths could have marked the evolution of the giant planets of our Solar system, assuming they suffered a temporary capture in the 2/1 resonance during the latest stages of the formation of our Solar system.

On S-matrix factorization of the Landau-Lifshitz model

We consider the three-particle scattering S-matrix for the Landau-Lifshitz model by directly computing the set of the Feynman diagrams up to the second order. We show, following the analogous computations for the non-linear Schrdinger model [1, 2], that the three-particle S-matrix is factorizable in the first non-trivial order.

O processo de execução orçamentária no governo do Estado do Maranhão: um estudo de caso na universidade estadual do Maranhão

Este estudo trata do processo de execução do orçamento, referente ao período de 1995 a 2008, da Universidade Estadual do Maranhão, órgão de natureza autárquica, vinculado à Secretaria de Estado da Ciência, Tecnologia, Educação Superior e Desenvolvimento Tecnológico. O objetivo central desta pesquisa foi verificar a existência de pressão orçamentária naquela Instituição e, se existente, demonstrar quais os critérios relevantes na alocação das cotas e quais elementos geram pressão na elaboração e execução do orçamento, através da análise de dados institucionais e entrevistas de servidores ligados à sua Administração Superior e controle orçamentário, mediante a comparação do que fora orçado com o efetivamente realizado, em seus grupos de despesas, ou seja, pessoal, custeio e capital. Para tanto, o problema desta pesquisa foi descrito através das seguintes questões: Há pressão orçamentária na UEMA, na fase de elaboração do orçamento? Há pressão orçamentária na UEMA, na fase de execução do orçamento? Que elementos geram pressão na elaboração e na execução do orçamento da UEMA? Quais são os critérios relevantes à alocação das cotas orçamentárias entre os Centros de Ensino da UEMA? A coleta de dados foi realizada através de entrevistas semi-estruturadas e documentos. O processo de análise de dados consistiu em verificar documentos referentes à dotação orçamentária comparativamente as cotas liberadas e a análise em profundidade dos depoimentos colhidos nas entrevistas. A discussão dos resultados gerou conclusões importantes por constatar a existência de pressão orçamentária na elaboração e na execução do orçamento daquela Universidade, identificando os elementos causadores da pressão, assim como os critérios relevantes na alocação das cotas.

Efeitos da prática de Yoga na memória e em parâmetros psicológicos e fisiológicos de indivíduos saudáveis

Techniques of mind & body control seem to benefit human organism in general and cognition in particular, because they involve a mindfulness practice. However, there is still a scarcity of studies with well-controlled methods to investigate the possible effects of Yoga practice. In this study, we investigated the effects of regular Yoga practice, based on Yoga postures (asanas), breathing techniques, and meditation exercises, on memory and physiologic and psychological parameters related to quality of life. There were significant improvements on performance tasks of short term memory and long term memory. We also observed significant beneficial effects on psychological and physiological parameters such as mood, anxiety, depression, stress, and modulation of the autonomic nervous system in Yoga practitioners group compared to the conventional physical exercises group. The results suggest the possible influences of stress, emotional state and mental training on cognitive effects of yoga practice. Our results support the indication of practice of Yoga for the treatment or prevention of stress, psychological disorders and their possible cognitive consequences

On the evection resonance and its connection to the stability of outer satellites

In terms of stability around the primary, it is widely known that the semimajor axis of the retrograde satellites is much larger than the corresponding semimajor axis of the prograde satellites. Usually this conclusion is obtained numerically, since precise analytical derivation is far from being easy, especially, in the case of two or more disturbers. Following the seminal idea that what is unstable in the restricted three-body problem is also unstable in the general N-body problem, we present a simplified model which allows us to derive interesting resonant configurations. These configurations are responsible for cumulative perturbations which can give birth to strong instability that may cause the ejection of the satellite. Then we obtain, analytically, approximate bounds of the stability of prograde and retrograde satellites. Although we recover quite well previous results of other authors, we comment very briefly some weakness of these bounds. Copyright (c) 2008 Tadashi Yokoyama et al.

On the stability of the satellites of asteroid 87 Sylvia

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Exploring S-type orbits in the Pluto-Charon binary system

This work generates, through a sample of numerical simulations of the restricted three-body problem, diagrams of semimajor axis and eccentricity which defines stable and unstable zones for particles in S-type orbits around Pluto and Charon. Since we consider initial conditions with 0 <= e <= 0.99, we found several new stable regions. We also identified the nature of each one of these newly found stable regions. They are all associated to families of periodic orbits derived from the planar circular restricted three-body problem. We have shown that a possible eccentricity of the Pluto-Charon system slightly reduces, but does not destroy, any of the stable regions.

Gravitational Capture of Asteroids by Gas Drag

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Irregular satellites of Jupiter: capture configurations of binary-asteroids

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Trabalho, corpo e subjetividade: toyotismo e formas de precariedade no capitalismo global

Nos últimos trinta anos de desenvolvimento capitalista, ocorreram transformações significativas nas diversas instâncias do ser social, com destaque para o mundo do trabalho e da reprodução social. Desenvolve-se o toyotismo, ideologia orgânica da nova produção capitalista, 'momento predominante' da reestruturação produtiva do capital. Sob o toyotismo, tende a constituir-se, pelo menos como 'promessa frustrada' do capital, o que iremos denominar 'compressão psicocorporal'. Esta constitui-se como um elemento da nova disposição sócio-subjetiva instaurada pelo toyotismo que caracteriza uma nova experiência do corpo, tanto no processo de trabalho quanto no processo sócio-reprodutivo.

Estatuto biológico do processamento de informação mental

Raciocinando no contexto do programa neomecanicista para a Biologia, estudamos a natureza do processamento de informação no sistema vivo em geral, e no cérebro humano em particular, onde uma aplicação do modelo da Auto-Organização nos conduz à hipótese do Supercódigo. Este seria um programa mental, molecularmente codificado, responsável pelas competências inatas, como a competência lingüística. Fazemos também uma comparação entre nossa hipótese e a da Linguagem do Pensamento, proposta por Jerry Fodor.

Nebular gas drag and co-orbital system dynamics

Aims. We study trajectories of planetesimals whose orbits decay due to gas drag in a primordial solar nebula and are perturbed by the gravity of the secondary body on an eccentric orbit whose mass ratio takes values from mu(2) = 10(-7) to mu(2) = 10(-3) increasing ten times at each step. Each planetesimal ultimately suffers one of the three possible fates: (1) trapping in a mean motion resonance with the secondary body; (2) collision with the secondary body and consequent increase of its mass; or (3) diffusion after crossing the orbit of the secondary body.Methods. We take the Burlirsh-Stoer numerical algorithm in order to integrate the Newtonian equations of the planar, elliptical restricted three-body problem with the secondary body and the planetesimal orbiting the primary. It is assumed that there is no interaction among planetesimals, and also that the gas does not affect the orbit of the secondary body.Results. The results show that the optimal value of the gas drag constant k for the 1: 1 resonance is between 0.9 and 1.25, representing a meter size planetesimal for each AU of orbital radius. In this study, the conditions of the gas drag are such that in theory, L4 no longer exists in the circular case for a critical value of k that defines a limit size of the planetesimal, but for a secondary body with an eccentricity larger than 0.05 when mu(2) = 10(-6), it reappears. The decrease of the cutoff collision radius increase the difusions but does not affect the distribution of trapping. The contribution to the mass accretion of the secondary body is over 40% with a collision radius 0.05R(Hill) and less than 15% with 0.005R(Hill) for mu(2) = 10(-7). The trappings no longer occur when the drag constant k reachs 30. That means that the size limit of planetesimal trapping is 0.2 m per AU of orbital radius. In most cases, this accretion occurs for a weak gas drag and small secondary eccentricity. The diffusions represent most of the simulations showing that gas drag is an efficient process in scattering planetesimals and that the trapping of planetesimals in the 1: 1 resonance is a less probable fate. These results depend on the specific drag force chosen.