O Grande Mentecapto: romance carnavalizado

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Análise da cintilação ionosférica no Brasil empregando GNSS e técnicas de mineração e visualização de dados

Pós-graduação em Ciências Cartográficas - FCT

Vozes de trabalhadores na ditadura civil-militar: ensaios sobre literatura, memória e testemunho

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Genealogia: da emergência às potencialidades contemporâneas

The article intends to articulate how the methodological proposal of Foucault, denominated genealogy, is applied to the field in which it emerged, considering that the proposal of this method appeared with the author’s study about the subject of the prisons. To apprehend the execution of the feathers in the contemporary epoch, we searched in Foucault’s theories the concepts of subjectivation processes, power relationships, discursive formations and dispositive. Starting from these concepts, we focused some practices and/or discursive formations of punishment and surveillance that happen at the present time to exemplify the form as the genealogical process raise an interlacement of subjects, information, appearances and disappearances that always obey to a normative logic. To unmask and to understand this logic can favor the liberation of manners of subjectivations crystallized in the punished people and in those ones that execute the punishment. Stiller, we question ourselves on which is the real function of the confinement, of the controls and, why not, if the paradigm of the modernity, the prison, had fail.

Diferença entre as espécies de Timbó (Derris Spp., Fabaceae) de diferentes regiões da Amazônia no controle da Musca domestica L.

The roots' powder of timbo species collected in different regions of Amazonia that were tested in larvae groupings, didn't produce differential significative effects in two strains of Musca domestica. The two species with the greater number of plants used in the trial were Derris urucu and Derris nicou; the individuals from the species came from regions considered as "forestal refugies" during the Amazonian pleistocene. Among each species the plants varied since that inefficient to control, until plants lethals to the fies. This differential capacity for larvae control among plants of the same species, originated from different regions, suggests that both species had their populations isolated, during the quaternary epoch. In regions or "forestal refugies", where both species were represented, D. urucu was superior to D. nicou in the capacity to control larvae. While among plants from F region (Peruvian-East refuge) of the State of Acre, the two species had convergence in the values of damage to larvae groupings. Among the another species, Derris sp. (yellow timbo or watermelon timbo) didn't show differences in larvae control between samples from the two regions; while the species that was introduced in the Amazonia Denis elleptica showed damage in the larvae groupings similar to the most effective plants of D. nicou and D. urucu.

Teores de rotenona em Clones de Timbó (Derris Spp. Fabaceae) de diferentes regiões da Amazônia e os seus efeitos na emergência de Imagos em Musca Domestica L

The rotenone contents analysis in clones of three timbó species permited the classification of these plants based on their efficiency to control Musca domestica larvae. The results showed significant correlations between the rotenone contents in the Derris urucu and D. nicou clones with the capacity to control the larvae. The plants with high rotenone contents were more effective. The rotenone contents, the effect of Derris species clones on the flics and the localization of the plants origin, showed that among the plants could have happened a populational isolation in the Amazonia during the pleistocene epoch. In Derris sp., that presented lower rotenone contents and was ineffective to control of the larvae, these differences were not observed.

O fantástico nos contos de Hoffmann e de Balzac: o artista louco

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Radarfacies and sedimentological analysis: study of sedimentary substrate from an archaeological site (shell mound), southern Brazil

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

A realidade virtual na humanidade atual

Virtual Reality it's present in our personal and professional daily life. Currently it comes been tested in many parameters. An example is, as an intervention mode related to healthy and rehabilitation field ( since phobias to physical problems ) due to dynamic interactive between human being and virtual reality, was able to be designed by a hardware and software integrated system. His appearance was in 1950s, through NASA's flight simulators in order to train astronauts in epoch (TORI et al.,2006).Subsequently, this began to expand to entertainment industry, where due to consumerism, only increasing his capacity to become so much more realist and reliable with the real environment. Because of this, beyond of your capacity be accessible which is low-cost, was used in scientific researches (motor area, physical aptitudes, cognitive, health, among others). The projected interactivity in this system type, in general, seek act according to people answers about the elements of virtual reality. Using the capacity that the reality is able to act of integrated way for human being. Following these concepts about virtual reality, the present study of literature revision, it comes as an purpose see humanity development. Since its birth, going on that point until your actuation and direct and indirect interplay in today's society from maturational form. Taking the concept of researchers' theory like Piaget. Following this line, the study will analyse how virtual reality might come to modify and act in social construction of society nowadays

A cyclic bipolar wind in the interacting binary V 393 Scorpii

V393 Scorpii is a double periodic variable characterized by a relatively stable non-orbital photometric cycle of 253 d. Mennickent et al. argue for the presence of a massive optically thick disc around the more massive B-type component and describe the evolutionary stage of the system. In this paper, we analyse the behaviour of the main spectroscopic optical lines during the long non-orbital photometric cycle. We study the radial velocity of the donor determining its orbital elements and find a small but significant orbital eccentricity (e = 0.04). The donor spectral features are modelled and removed from the spectrum at every observing epoch using the light-curve model given by Mennickent et al. We find that the line emission is larger during eclipses and mostly comes from a bipolar wind. We also find that the long cycle is explained in terms of a modulation of the wind strength; the wind has a larger line and continuum emissivity at the high state. We report the discovery of highly variable chromospheric emission in the donor, as revealed by the Doppler maps of the emission lines Mg II 4481 and C I 6588. We discuss notable and some novel spectroscopic features like discrete absorption components, especially visible at blue depressed O I 7773 absorption wings during the second half-cycle, Balmer double emission with V/R curves showing 'Z-type' and 'S-type' excursions around secondary and main eclipses, respectively, and H beta emission wings extending up to +/- 2000 km s(-1). We also discuss possible causes for these phenomena and for their modulations with the long cycle.

Particle creation due to tachyonic instability in relativistic stars

Dense enough compact objects were recently shown to lead to an exponentially fast increase of the vacuum energy density for some free scalar fields properly coupled to the spacetime curvature as a consequence of a tachyonic-like instability. Once the effect is triggered, the star energy density would be overwhelmed by the vacuum energy density in a few milliseconds. This demands that eventually geometry and field evolve to a new configuration to bring the vacuum back to a stationary regime. Here, we show that the vacuum fluctuations built up during the unstable epoch lead to particle creation in the final stationary state when the tachyonic instability ceases. The amount of created particles depends mostly on the duration of the unstable epoch and final stationary configuration, which are open issues at this point. We emphasize that the particle creation coming from the tachyonic instability will occur even in the adiabatic limit, where the spacetime geometry changes arbitrarily slowly, and therefore is quite distinct from the usual particle creation due to the change in the background geometry.

GEOGRAPHICAL GENETIC STRUCTURING AND PHENOTYPIC VARIATION IN THE VELLOZIA HIRSUTA (VELLOZIACEAE) OCHLOSPECIES COMPLEX

Premise of the study: Vellozia hirsuta forms a complex presenting wide morphological and anatomical variation, resulting in five specific names and 14 morpho-anatomical patterns occurring in disjunct populations. We carried out a phylogeographical study to investigate the existence of correlation among the genetic and morphological patterns within this complex, and to determine whether it is composed of various species or should be treated as an ochlospecies, a species having widely polymorphic and weakly polytypic complex variation, with morphological characteristics varying independently. Methods: We carried out phylogeographical analyses using cpDNA rpl32F-trnL intergenic region. Key results: We found 20 haplotypes in 23 populations sampled. The populations are genetically structured (Phi(ST) = 0.818) into four phylogeographical groups demonstrating geographical structuring but with no correlation with morpho-anatomical patterns. Our analyses do not support recognizing any of the species now synonymized under Vellozia hirsuta. The northern populations were the most genetically differentiated and could be considered a distinct taxon, as they are also morphologically different. Conclusions: It is recommended that Vellozia hirsuta be considered a single enormously variable species. The patterns of variation within V. hirsuta probably are related to climatic changes that occurred during the Pleistocene Epoch in tropical Brazil when reductions in forest cover favored the expansion of V. hirsuta populations into extensive lowland areas. The expansion of forest cover at the end of the glaciations would have again restricted the occurrence of campos rupestres vegetation to high elevations, which constitute the current centers of diversity of this species.

Transiting exoplanets from the CoRoT space mission XXI. CoRoT-19b: a low density planet orbiting an old inactive F9V-star

Context. Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. These measurements indicate that planets of similar mass can have very different radii. For low-density planets, it is generally assumed that they are inflated owing to their proximity to the host-star. To determine the causes of this inflation, it is necessary to obtain a statistically significant sample of planets with precisely measured masses and radii. Aims. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. Methods. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. Results. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M-* = 1.21 +/- 0.05 M-circle dot and radius R-* = 1.65 +/- 0.04 R-circle dot. The planet has a mass of M-P = 1.11 +/- 0.06 M-Jup and radius of R-P = 1.29 +/- 0.03 R-Jup. The resulting bulk density is only rho = 0.71 +/- 0.06 g cm (3), which is much lower than that for Jupiter. Conclusions. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a approximate to 30% larger radius.

New activity in the large circumstellar disk of the Be-shell star 48 Librae

Aims. Spectroscopic, polarimetric, and high spectral resolution interferometric data covering the period 1995-2011 are analyzed to document the transition into a new phase of circumstellar disk activity in the classical Be-shell star 48 Lib. The objective is to use this broad data set to additionally test disk oscillations as the basic underlying dynamical process. Methods. The long-term disk evolution is described using the V/R ratio of the violet and red emission components of H alpha and Br gamma, radial velocities and profiles of He I and optical metal shell lines, as well as multi-band BVRI polarimetry. Single-epoch broad-band and high-resolution interferometric visibilities and phases are discussed with respect to a classical disk model and the given baseline orientations. Results. Spectroscopic signatures of disk asymmetries in 48 Lib vanished in the late nineties but recovered some time between 2004 and 2007, as shown by a new large-amplitude and long-duration V/R cycle. Variations in the radial velocity and line profile of conventional shell lines correlate with the V/R behavior. They are shared by narrow absorption cores superimposed on otherwise seemingly photospheric He I lines, which may form in high-density gas at the inner disk close to the photosphere. Large radial velocity variations continued also during the V/R-quiet years, suggesting that V/R may not always be a good indicator of global density waves in the disk. The comparison of the polarization after the recovery of the V/R activity shows a slight increase, while the polarization angle has been constant for more than 20 years, placing tight limits on any 3-D precession or warping of the disk. The broad H-band interferometry gives a disk diameter of (1.72 +/- 0.2) mas (equivalent to 15 stellar radii), position angle of the disk (50 +/- 9)degrees and a relatively low disk flattening of 1.66 +/- 0.3. Within the errors the same disk position angle is derived from polarimetric observations and from photocenter shifts across Br gamma. The high-resolution interferometric visibility and phase profiles show a double or even multiple-component structure. A preliminary estimate based on the size of the Br gamma emitting region indicates a large diameter for the disk (tens of stellar radii). Overall, no serious contradiction between the observations and the disk-oscillation model could be construed.

The Gemini planet-finding campaign: the frequency of giant planets aroud debris disk stars

We have completed a high-contrast direct imaging survey for giant planets around 57 debris disk stars as part of the Gemini NICI Planet-Finding Campaign. We achieved median H-band contrasts of 12.4 mag at 0.''5 and 14.1 mag at 1'' separation. Follow-up observations of the 66 candidates with projected separation <500 AU show that all of them are background objects. To establish statistical constraints on the underlying giant planet population based on our imaging data, we have developed a new Bayesian formalism that incorporates (1) non-detections, (2) single-epoch candidates, (3) astrometric and (4) photometric information, and (5) the possibility of multiple planets per star to constrain the planet population. Our formalism allows us to include in our analysis the previously known β Pictoris and the HR 8799 planets. Our results show at 95% confidence that <13% of debris disk stars have a ≥5 M Jup planet beyond 80 AU, and <21% of debris disk stars have a ≥3 M Jup planet outside of 40 AU, based on hot-start evolutionary models. We model the population of directly imaged planets as d 2 N/dMdavpropm α a β, where m is planet mass and a is orbital semi-major axis (with a maximum value of a max). We find that β < –0.8 and/or α > 1.7. Likewise, we find that β < –0.8 and/or a max < 200 AU. For the case where the planet frequency rises sharply with mass (α > 1.7), this occurs because all the planets detected to date have masses above 5 M Jup, but planets of lower mass could easily have been detected by our search. If we ignore the β Pic and HR 8799 planets (should they belong to a rare and distinct group), we find that <20% of debris disk stars have a ≥3 M Jup planet beyond 10 AU, and β < –0.8 and/or α < –1.5. Likewise, β < –0.8 and/or a max < 125 AU. Our Bayesian constraints are not strong enough to reveal any dependence of the planet frequency on stellar host mass. Studies of transition disks have suggested that about 20% of stars are undergoing planet formation; our non-detections at large separations show that planets with orbital separation >40 AU and planet masses >3 M Jup do not carve the central holes in these disks.