A clínica da psicofísica

Apresentamos a Psicofísica como uma ciência aplicada nas investigações e nas abordagens e diagnósticos clínicos. Inicialmente, introduzimos algo dos aspectos epistemológicos e teóricos da área, passamos para as abordagens que a Psicofísica pode apresentar na aplicabilidade clínica e, por fim, discutimos os avanços recentes da aplicação clínica, apresentamos as experiências de nosso laboratório de pesquisa clínica em psicofísica, finalizando com as perspectivas de ampliação do uso da psicofísica para investigações clínicas de funções perceptuais mais complexas.

Corporeidade e ação nos processos de formação do eu

Parte-se da hipótese de que tanto os modos de constituição da subjetividade, quanto as teses epistemológicas sobre a formação do eu têm sofrido importantes mudanças nas últimas décadas. No plano das identidades pessoais, tal fato se expressa no atenuamento do ideário intimista, tradicionalmente centrado na idéia da vida mental como espaço privado e interior. No plano epistemológico, diferentes saberes vêm questionando a equivalência entre vida mental e interioridade psicológica e propondo descrições da origem do eu que incluam a dimensão da corporeidade e da ação. Considerando as noções de representação e de ação como eixos fundamentais para diferentes concepções da subjetividade, este artigo examina um modelo internalista do psiquismo, contrastando-o com outro que toma o eu como agente corporificado.

Incidências da hermenêutica para a metodologia da pesquisa teórica em psicanálise

O artigo traz uma breve revisão das principais abordagens hermenêuticas envolvidas na interpretação de textos e discursos a fim de delimitar a incidência dessa problemática no campo da pesquisa teórica em psicanálise. Define as diferentes formas de pesquisa em psicanálise e indica como as mudanças na compreensão da hermenêutica incidem também sobre a compreensão do estatuto epistemológico do saber psicanalítico. Apresenta e discute as propostas de metodologia de investigação teórica de Laplanche e Figueiredo. Ao concluir, indica a aproximação do método psicanalítico aplicado a textos e discursos com as perspectivas contemporâneas da hermenêutica e propõe uma abordagem própria para pesquisas de cunho histórico-conceitual e epistemológico em psicanálise.

Razão e desrazão nas tomadas de decisão

Tal como se apresenta na atualidade, o campo de Teorias de Tomadas de Decisão reflete a intersecção de três desenvolvimentos teóricos principais: Utilidade Esperada, Heurísticas e Desvios e Intuição Holística. As relações entre estes não são clarividentes, nem estão estabelecidas na literatura sobre o assunto, sobretudo porque algumas das tendências em jogo ainda são muito novas. Meu objetivo é contribuir para o suprimento desta lacuna, oferecendo uma visão geral do campo, particularmente sensível às demandas epistemológicas às quais cada novo desenvolvimento respondeu e às limitações destas respostas. De especial interesse é o fato de que isto irá habilitar o leitor a compreender os fundamentos do novo conceito de intuição decisional que desponta e a se posicionar criticamente em relação ao mesmo.

Paradigmas, eixos temáticos e tensões na PTO no Brasil

O panorama de abordagens da psicologia do trabalho e das organizações (PTO) no Brasil mostra grande diversidade teórica e metodológica que reflete a presença de distintos paradigmas científicos na delimitação e organização desse campo. O objetivo deste artigo é analisar esses paradigmas e relacioná-los com três eixos temáticos da PTO no Brasil: o do comportamento, o da subjetividade e o clínico. Investiga-se os fundamentos epistemológicos e metodológicos, alguns trabalhos e autores de cada um desses eixos, discutindo sua contribuição para o campo da PTO no Brasil. O artigo desenvolve uma discussão sobre as tensões existentes entre esses eixos, derivadas da pressão de corresponderem, ao mesmo tempo, a critérios de rigor acadêmico e relevância organizacional. O artigo, por fim, mostra a diversificação do campo da PTO no Brasil e os desafios disso decorrentes.

Promoção da saúde: elemento instituinte?

O artigo inclui na discussão sobre os resultados da promoção da saúde um argumento de natureza epistemológica, levando em consideração o contexto contemporâneo de mudanças econômicas, políticas e culturais do qual ela é parte e expressão. Destacam-se, por um lado, as suspeitas que recaem sobre o projeto da Modernidade, sejam elas decorrentes do crescimento das incertezas ou da irrealização de promessas e, por outro lado, as tentativas de equacionamento do binômio determinação/autonomia, como questões sensíveis a uma ruptura dos modos de conhecer na contemporaneidade. Propõe-se considerar a dinâmica social e abordá-la como a união e a tensão da história feita e da história se fazendo, para melhor compreender o alcance e os resultados da promoção da saúde. A conclusão é que a promoção da saúde deve continuar buscando o desenvolvimento de ações cada vez mais efetivas, mas deve fazê-lo sem abdicar da possibilidade de manter-se próxima da energia social livre e em ebulição, que caracteriza o elemento instituinte de uma produção histórica.

The Staircase Structure of the Southern Brazilian Continental Shelf

We show some evidences that the Southeastern Brazilian Continental Shelf (SBCS) has a devil's staircase structure, with a sequence of scarps and terraces with widths that obey fractal formation rules. Since the formation of these features is linked with the sea-level variations, we say that the sea level changes in an organized pulsating way. Although the proposed approach was applied in a particular region of the Earth, it is suitable to be applied in an integrated way to other shelves around the world, since the analyses favor the revelation of the global sea-level variations. Copyright (C) 2009 M. S. Baptista and L. A. Conti.

A institucionalização da ciência da informação no Brasil sob a ótica da evolução quantitativa dos cursos de graduação na área

The study describes the process of scientific institutionalization of Information Science in Brazil, from quantitative analysis of the development of undergraduate courses in the area. As body of research, it considers the following courses: Librarianship, Archival Science, Museology, Information Science and Management one, created between the years 1910 and 2008. It is noted that the growth trend of the quantity of courses reflects the importance given to information in the current context. However, the diversity of nomenclature and conceptual differences in the theoretical field illustrate the epistemological fragility of the area, as well as the search for greater professional visibility in society.

The structure and dynamics of Abell 1942

Aims. We present a dynamical analysis of the galaxy cluster Abell 1942 based on a set of 128 velocities obtained at the European Southern Observatory. Methods. Data on individual galaxies are presented and the accuracy of the determined velocities as some properties of the cluster are discussed. We have also made use of publicly available Chandra X-ray data. Results. We obtained an improved mean redshift value z = 0.22513 +/- 0.0008 and velocity dispersion sigma = 908(139)(+147) km s(-1). Our analysis indicates that inside a radius of similar to 1.5 h(70)(-1) Mpc (similar to 7 arcmin) the cluster is well relaxed, without any remarkable features and the X-ray emission traces the galaxy distribution fairly well. Two possible optical substructures are seen at similar to 5 arcmin from the centre in the northwest and the southwest directions, but are not confirmed by the velocity field. These clumps are, however, kinematically bound to the main structure of Abell 1942. X-ray spectroscopic analysis of Chandra data resulted in a temperature kT = 5.5+/-0.5 keV and metal abundance Z = 0.33 +/- 0.15 Z(circle dot). The velocity dispersion corresponding to this temperature using the T(X-sigma) scaling relation is in good agreement with the measured galaxy velocities. Our photometric redshift analysis suggests that the weak lensing signal observed to the south of the cluster and previously attributed to a ""dark clump"" is produced by background sources, possibly distributed as a filamentary structure.

Fossil groups in the Millennium Simulation Evolution of the brightest galaxies

Aims. We create a catalogue of simulated fossil groups and study their properties, in particular the merging histories of their first-ranked galaxies. We compare the simulated fossil group properties with those of both simulated non-fossil and observed fossil groups. Methods. Using simulations and a mock galaxy catalogue, we searched for massive (>5 x 10(13) h(-1) M-circle dot) fossil groups in the Millennium Simulation Galaxy Catalogue. In addition, we attempted to identify observed fossil groups in the Sloan Digital Sky Survey Data Release 6 using identical selection criteria. Results. Our predictions on the basis of the simulation data are: (a) fossil groups comprise about 5.5% of the total population of groups/clusters with masses larger than 5 x 10(13) h(-1) M-circle dot. This fraction is consistent with the fraction of fossil groups identified in the SDSS, after all observational biases have been taken into account; (b) about 88% of the dominant central objects in fossil groups are elliptical galaxies that have a median R-band absolute magnitude of similar to-23.5-5 log h, which is typical of the observed fossil groups known in the literature; (c) first-ranked galaxies of systems with M > 5 x 10(13) h(-1) M-circle dot, regardless of whether they are either fossil or non-fossil, are mainly formed by gas-poor mergers; (d) although fossil groups, in general, assembled most of their virial masses at higher redshifts in comparison with non-fossil groups, first-ranked galaxies in fossil groups merged later, i.e. at lower redshifts, compared with their non-fossil-group counterparts. Conclusions. We therefore expect to observe a number of luminous galaxies in the centres of fossil groups that show signs of a recent major merger.

The qWR star HD 45166 - II. Fundamental stellar parameters and evidence of a latitude-dependent wind

Context. The enigmatic object HD 45166 is a qWR star in a binary system with an orbital period of 1.596 day, and presents a rich emission-line spectrum in addition to absorption lines from the companion star (B7 V). As the system inclination is very small (i = 0.77 degrees +/- 0.09 degrees), HD 45166 is an ideal laboratory for wind-structure studies. Aims. The goal of the present paper is to determine the fundamental stellar and wind parameters of the qWR star. Methods. A radiative transfer model for the wind and photosphere of the qWR star was calculated using the non-LTE code CMFGEN. The wind asymmetry was also analyzed using a recently-developed version of CMFGEN to compute the emerging spectrum in two-dimensional geometry. The temporal-variance spectrum (TVS) was calculated to study the line-profile variations. Results. Abundances and stellar and wind parameters of the qWR star were obtained. The qWR star has an effective temperature of T(eff) = 50 000 +/- 2000 K, a luminosity of log(L/L(circle dot)) = 3.75 +/- 0.08, and a corresponding photospheric radius of R(phot) = 1.00 R(circle dot). The star is helium-rich (N(H)/N(He) = 2.0), while the CNO abundances are anomalous when compared either to solar values, to planetary nebulae, or to WR stars. The mass-loss rate is. M = 2.2 x 10(-7) M(circle dot) yr(-1), and the wind terminal velocity is v(infinity) = 425 km s(-1). The comparison between the observed line profiles and models computed under different latitude-dependent wind densities strongly suggests the presence of an oblate wind density enhancement, with a density contrast of at least 8: 1 from equator to pole. If a high velocity polar wind is present (similar to 1200 km s(-1)), the minimum density contrast is reduced to 4:1. Conclusions. The wind parameters determined are unusual when compared to O-type stars or to typical WR stars. While for WR stars v(infinity)/v(esc) > 1.5, in the case of HD 45166 it is much smaller (v(infinity)/v(esc) = 0.32). In addition, the efficiency of momentum transfer is eta = 0.74, which is at least 4 times smaller than in a typical WR. We find evidence for the presence of a wind compression zone, since the equatorial wind density is significantly higher than the polar wind. The TVS supports the presence of such a latitude-dependent wind and a variable absorption/scattering gas near the equator.

Turbulent magnetic pumping in a Babcock-Leighton solar dynamo model

Context. The turbulent pumping effect corresponds to the transport of magnetic flux due to the presence of density and turbulence gradients in convectively unstable layers. In the induction equation it appears as an advective term and for this reason it is expected to be important in the solar and stellar dynamo processes. Aims. We explore the effects of turbulent pumping in a flux-dominated Babcock-Leighton solar dynamo model with a solar-like rotation law. Methods. As a first step, only vertical pumping has been considered through the inclusion of a radial diamagnetic term in the induction equation. In the second step, a latitudinal pumping term was included and then, a near-surface shear was included. Results. The results reveal the importance of the pumping mechanism in solving current limitations in mean field dynamo modeling, such as the storage of the magnetic flux and the latitudinal distribution of the sunspots. If a meridional flow is assumed to be present only in the upper part of the convective zone, it is the full turbulent pumping that regulates both the period of the solar cycle and the latitudinal distribution of the sunspot activity. In models that consider shear near the surface, a second shell of toroidal field is generated above r = 0.95 R(circle dot) at all latitudes. If the full pumping is also included, the polar toroidal fields are efficiently advected inwards, and the toroidal magnetic activity survives only at the observed latitudes near the equator. With regard to the parity of the magnetic field, only models that combine turbulent pumping with near-surface shear always converge to the dipolar parity. Conclusions. This result suggests that, under the Babcock-Leighton approach, the equartorward motion of the observed magnetic activity is governed by the latitudinal pumping of the toroidal magnetic field rather than by a large scale coherent meridional flow. Our results support the idea that the parity problem is related to the quadrupolar imprint of the meridional flow on the poloidal component of the magnetic field and the turbulent pumping positively contributes to wash out this imprint.

Searching for star formation outside galaxies: Multiwavelength analysis of the intragroup medium of Hickson Compact Group 100

We use multiwavelength data (H I, FUV, NUV, R) to search for evidence of star formation in the intragroup medium of the Hickson Compact Group 100. We find that young star-forming regions are located in the intergalactic H I clouds of the compact group which extend to over 130 kpc away from the main galaxies. A tidal dwarf galaxy (TDG) candidate is located in the densest region of the H I tail, 61 kpc from the brightest group member and its age is estimated to be only 3.3 Myr. Fifteen other intragroup H II regions and TDG candidates are detected in the Galaxy Evolution Explorer (GALEX) FUV image and within a field 10' x 10' encompassing the H I tail. They have ages <200 Myr, H I masses of 10(9.2-10.4) M(circle dot), 0.001 circle dot) yr(-1), and stellar masses 10(4.3)-10(6.5) M(circle dot). The H I clouds to which many of them are associated have column densities about one order of magnitude lower than N(H I) similar to 10(21) cm(-2).

First stars XIII. Two extremely metal-poor RR Lyrae stars

Context. The chemical composition of extremely metal-poor stars (EMP stars; [Fe/H] < similar to -3) is a unique tracer of early nucleosynthesis in the Galaxy. As such stars are rare, we wish to find classes of luminous stars which can be studied at high spectral resolution. Aims. We aim to determine the detailed chemical composition of the two EMP stars CS 30317-056 and CS 22881-039, originally thought to be red horizontal-branch (RHB) stars, and compare it to earlier results for EMP stars as well as to nucleosynthesis yields from various supernova (SN) models. In the analysis, we discovered that our targets are in fact the two most metal-poor RR Lyrae stars known. Methods. Our detailed abundance analysis, taking into account the variability of the stars, is based on VLT/UVES spectra (R similar or equal to 43 000) and 1D LTE OSMARCS model atmospheres and synthetic spectra. For comparison with SN models we also estimate NLTE corrections for a number of elements. Results. We derive LTE abundances for the 16 elements O, Na, Mg, Al, Si, S, Ca, Sc, Ti, Cr, Mn, Fe, Co, Ni, Sr and Ba, in good agreement with earlier values for EMP dwarf, giant and RHB stars. Li and C are not detected in either star. NLTE abundance corrections are newly calculated for O and Mg and taken from the literature for other elements. The resulting abundance pattern is best matched by model yields for supernova explosions with high energy and/or significant asphericity effects. Conclusions. Our results indicate that, except for Li and C, the surface composition of EMP RR Lyr stars is not significantly affected by mass loss, mixing or diffusion processes; hence, EMP RR Lyr stars should also be useful tracers of the chemical evolution of the early Galactic halo. The observed abundance ratios indicate that these stars were born from an ISM polluted by energetic, massive (25-40 M(circle dot)) and/or aspherical supernovae, but the NLTE corrections for Sc and certain other elements do play a role in the choice of model.

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4+/-0.3 mu Hz and angular and linear radiuses of 0.6759 +/- 0.0062 mas and 1.010 +/- 0.009 R(circle dot) were estimated. We used these values to derive the mass of the star, 1.02 +/- 0.03 M(circle dot).