Sentidos do trabalho informacional corporativo: uma investigação sobre o impacto do conhecimento no trabalho contemporâneo

This study proposes and uses a multipolar qualitative methodology for the investigation of the meanings of corporate work under the impact of the technical-scientific knowledge. Based on the constructionist epistemology and on a heideggerian approach, this methodology made possible the description of such phenomenon under the Management perspective, but also under the Psychology, Sociology and Philosophy views. Study starts with empirical data, collected by interviews and in publications, and analyzes them based on conceptual contributions from the four referred poles. As a result, this investigation proposes reflexivity, impermanence and entanglement as meanings of the corporate work that culminate in the paradoxical work. It also demonstrates that the impact of knowledge occurs in a reflexive spiral of complexification, continuously affecting individuals and work processes; describes the impermanent character of the work ruled by time, by neophilia and by uncertainties that make precarious the very subjective experience of worker; and proposes that this work becomes entangled due to the way it is managed, and is an entangling work, for embarrassing the individual in its techniques, logics and dissonances. The paradoxical essence that emerges from this appreciation of corporate work is described on the following scopes: its reflexivity does not prevent its rationality to be fragile; its dynamism coexists with the difficulty to achieve substantive organizational changes; its entanglement compromises the possibilities of an apparently reachable well-being; its focus on present ends up to be emptied; and its purpose of individual sustenance becomes unsustainable due to hyperconsumption. But the conclusions of the study do no describe a definitive phenomenon. At the ending, it points out possibilities of living with the paradoxical work as well as possibilities of its transformation.

Análise de diagramas cor-magnitude de 5 aglomerados ricos da LMC

Apresentamos a análise de diagramas cor-magnitude (CMDs) profundos para 5 aglomerados ricos da Grande Nuvem de Magalhães (LMC). Os dados fazem parte do projeto HST G07307, entitulado "Formação e Evolução de Aglomerados Estelares Ricos da LMC", e foram obtidos através do HST/WFPC2 nos filtros F555W (~ V) e F814W (~ I), alcançando V555~25. A amostra de aglomerados é composta por NGC 1805 e NGC 1818, os mais jovens (r < 100 Myr), NGC 1831e NGC 1868,de idades intermediárias (400 < r < 1000Myr), e Hodge 14, o mais velho (r > 1200Myr). Discutimos e apresentamos um método de correção dos CMDs para incompleteza da amostra e contaminação por estrelas de campo. O uso eficiente das informações contidas nos CMDs foi feito por meio de comparações entre os CMDs observados e CMDs modelados. O processo de modelamento de CMDs gera uma Seqüência Principal (MS) sintética, que utiliza como entrada do modelo a informação sobre idade (r), metalicidade (Z), Função de Massa do Presente (PDMF), fração de binárias não resolvidas, distância e extinção da luz. As incertezas fotométricas foram empiricamente determinadas a partir dos dados e incorporadas no modelamento. Técnicas estatísticas de comparação entre CMDs em 1D e 2D são apresentadas e aplicadas como métodos objetivos capazes de determinar a compatibilidade entre modelo e observação. Modelando os CMDs da região central dos aglomerados podemos inferir a metalicidade (Z), o módulo de distância intrínseco ((V - Mv)o) e o avermelhamento (E(B-V)) para cada aglomerado. Também determinamos as idades para os 3 aglomerados mais velhos de nossa amostra. Continuação) Através da comparação em 2D os valores encontrados foram os seguintes: para NGC 1805, Z = 0.007:1+-0.003, (V - Mv)o = 18.50:1+- 0.10, E(B - V) = 0.03:1+-0.01; para NGC 1818,Z = 0.005:1+-0.002, (V - Mv)o = 18.50:1+-0.15, E(B - V)~0.00; para NGC 1831, Z = 0.012:1+-0.002, log(r /yr) = 8.70 :I+-0.05, (V - Mv)o = 18.70:1+- 0.05, E(B - V)~ 0.00; para NGC 1868, Z = 0.008:1+-0.002,log(r/yr) =8.95:1+-0.05, (V - Mv)o = 18.70:1+- 0.05, E(B - V) ~0.00; para Hodge 14, Z = 0.008+-0.004, log(r/yr) = 9.23+-0.10, (V - Mv)o = 18.50+-0.15, E(B - V) = 0.02+- 0.02. Estes valores estão de acordo, dentro das incertezas, com os valores obtidos através da análise de linhas fiduciais (lD), o que agrega confiabilidade a estas determinações. Através da análise de CMDs em regiões concêntricas determinamos a dependência espacial da inclinação da PDMF (a) nos aglomerados mais ricos. Para tanto empregamos duas abordagens distintas para a determinação de a: 1) método tradicional em 1D via conversão direta de V555em massa; 2) método em 2D via modelmento de CMDs. Independente do método de análise, todos os aglomerados analisados demonstram claramente o efeito de segregação em massa. Além disso, NGC 1818, NGC 1831 e NGC 1868 apresentam uma possível perda seletiva de estrelas de baixa massa nas suas regiões mais externas.

Capital social: vários conceitos, um só problema

Esta dissertação discute capital social, um tema relativamente novo nas ciências humanas, mas que está diretamente relacionado com um velho problema da vida social: os dilemas da ação coletiva, isto é, como uma sociedade pode desenvolver-se por meio de confiança mútua entre seus membros e cooperação em torno de objetivos comuns, evitando os velhos problemas envolvendo bens públicos, quais sejam, os “caronas” e as atitudes “caçadoras de renda”. Em primeiro lugar, situa-se a discussão enfocando o problema da ação coletiva de um enfoque mais amplo: os dilemas da cooperação, as ações altruístas e seu suposto conflito com um modelo de ser humano movido pelo auto-interesse, o pressuposto da economia neoclássica do “homem econômico” e, enfim, a teoria da lógica da ação coletiva e suas limitações. Em segundo lugar, apontam-se as 4 principais correntes de pensamento que buscam definir o conceito de capital social: o comunitarismo de Tocqueville e Putnam, o capital social como gerador de capital humano de Coleman, o capital social no mercado das trocas simbólicas de Bourdieu e, por último, o capital social como infra-estrutura social (instituições) de North. Por último, são apresentados casos de aplicação dos conceitos de capital social baseados em trabalhos teórico-analíticos e de observações empíricas em diversos países, mostrando-se as diferentes formas que ele pode assumir conforme o contexto em que é analisado e, sobretudo, os efeitos que ele pode produzir numa comunidade, numa região ou mesmo num país inteiro.

Estágios iniciais de aglomerados estelares

Analisamos aglomeradosimersosem nuvens moleculares, os quais são fundamentais para a compreensão dos estágios evolutivos iniciais da formação estelar. Na presente tese exploramos principalmente objetos associados a nebulosas de reflexão. Os objetos que estão no foco central do nosso estudo são possíveis aglomerados presentes na direção de nebulosas de reflexãoou emissão,já apontados pelos trabalhos de Bica et aI. (2003b) e Dutra et alo (2003). No estudo desses sistemas utilizamos principalmente dados do Catálogo 2MASS. A análise fotométrica é baseada em diagramas cor-magnitude e cor-cor, juntamente com isócronas teóricas de pré-seqüência-principaI. A distribuição angular de densidade superficial de estrelas no aglomerado e no campo próximo é um outro método de análise utilizado. Através da análise fotométrica e espectroscópica obtivemos os parâmetros físicos fundamentais dos aglomerados. Com base na emissão de estrelas na banda Ks realizamos uma busca por novos aglomerados imersos. A busca foi orientada na direção central de 47 nebulosas no ótico selecionadas a partir do Catálogo de Dutra et aI. (2003), varrendo um raio angular de r = 10' para cada direção. A busca resultou na descoberta de um aglomerado imerso ainda não catalogado, e aqueles já catalogados foram redescobertos. Neste trabalho obtivemos parâmetros físicos para mais de 30 aglomerados imersos. O raio linear derivado para esses objetos situa-se na faixa de 0,3 a 0,9 pc e o número de estrelas membros detectadas fica geralmente na faixa de 20 a 50 A idade média derivada para a amostra indica uma população bastante jovem. A maior parte dos aglomerados possui uma idade de 1 a 2 milhões de anos. Em nossa amostra o objeto mais massivo encontrado possui uma massa estimada de ~ 200M<=).Entretanto, a maioria dos aglomerados possui massa estimada na faixa de ~ 20M<=)a ~ 60M<=).Os valores de massa total para cada aglomerado não possuem uma correlação aparente com o ambiente da nebulosa. Os aglomerados imersos associados a nebulosas em ambientes de complexo HII podem apresentar massas tão baixas quanto aqueles associados a nebulosas de reflexão. Estes sistemas estelares provavelmente não apresentam estrelas com massas superiores àquela de uma estrela com tipo espectral B. Finalmente, estudamos um aglomerado imerso contendo uma estrela OV, o aglomerado NGC 2264. Obtivemos uma função de massa inicial (FMI) para o aglomerado NGC 2264 a partir de 346 fontes de raio-X detectadas pelo CHANDRA com contrapartida no infra-vermelho. A FMI derivada inclui massas estelares acima de M = O,03M<=). Em comparação com a FMI da vizinhança solar existe uma deficiência de estrelas de baixa massa para M < O,3M<=). As massas estimadas para os objetos analisados indicam que eles são sistemas estelares não-ligados gravitacionalmente. A maioria dos aglomerados de nossa amostra possui massa inferior a 100M<=)e está associada a nebulosas de reflexão. A formação de estrelas do tipo O em aglomerados imersos não-ligados gravitacionalmente não parece ser freqüente, segundo nossos resultados.

The possibility of primordial black hole direct detection

This thesis explores the possibility of directly detecting blackbody emission from Primordial Black Holes (PBHs). A PBH might form when a cosmological density uctuation with wavenumber k, that was once stretched to scales much larger than the Hubble radius during ination, reenters inside the Hubble radius at some later epoch. By modeling these uctuations with a running{tilt power{law spectrum (n(k) = n0 + a1(k)n1 + a2(k)n2 + a3(k)n3; n0 = 0:951; n1 = ????0:055; n2 and n3 unknown) each pair (n2,n3) gives a di erent n(k) curve with a maximum value (n+) located at some instant (t+). The (n+,t+) parameter space [(1:20,10????23 s) to (2:00,109 s)] has t+ = 10????23 s{109 s and n+ = 1:20{2:00 in order to encompass the formation of PBHs in the mass range 1015 g{1010M (from the ones exploding at present to the most massive known). It was evenly sampled: n+ every 0.02; t+ every order of magnitude. We thus have 41 33 = 1353 di erent cases. However, 820 of these ( 61%) are excluded (because they would provide a PBH population large enough to close the Universe) and we are left with 533 cases for further study. Although only sub{stellar PBHs ( 1M ) are hot enough to be detected at large distances we studied PBHs with 1015 g{1010M and determined how many might have formed and still exist in the Universe. Thus, for each of the 533 (n+,t+) pairs we determined the fraction of the Universe going into PBHs at each epoch ( ), the PBH density parameter (PBH), the PBH number density (nPBH), the total number of PBHs in the Universe (N), and the distance to the nearest one (d). As a rst result, 14% of these (72 cases) give, at least, one PBH within the observable Universe, one{third being sub{stellar and the remaining evenly spliting into stellar, intermediate mass and supermassive. Secondly, we found that the nearest stellar mass PBH might be at 32 pc, while the nearest intermediate mass and supermassive PBHs might be 100 and 1000 times farther, respectively. Finally, for 6% of the cases (four in 72) we might have substellar mass PBHs within 1 pc. One of these cases implies a population of 105 PBHs, with a mass of 1018 g(similar to Halley's comet), within the Oort cloud, which means that the nearest PBH might be as close as 103 AU. Such a PBH could be directly detected with a probability of 10????21 (cf. 10????32 for low{energy neutrinos). We speculate in this possibility.

Nitretação em plasma com gaiola catódica: investigação do mecanismo e estudo comparativo com a nitretação em plasma de tensão contínua

The ionic plasma nitriding is one of the most important plasma assisted treatment technique for surface modification, but it presents some inherent problems mainly in nitriding pieces with complex geometries. In the last four years has appeared a plasma nitriding technique, named ASPN (Active Screen Plasma Nitriding) in which the samples and the workload are surrounded by a metal screen on which the cathodic potential is applied. This new technique makes possible to obtain a perfect uniform nitrided layer apart from the shape of the samples. The present work is based on the development of a new nitriding plasma technique named CCPN (Cathodic Cage Plasma Nitriding) Patent PI 0603213-3 derived from ASPN, but utilizes the hollow cathode effect to increase the nitriding process efficiency. That technique has shown great improvement on the treatment of several types of steels under different process conditions, producing thicker and harder layers when compared with both, ASPN and ionic plasma nitriding, besides eliminating problems associated with the later technique. The best obtained results are due to the hollow cathode effect on the cage holes. Moreover, characteristic problems of ionic plasma nitriding are eliminated due to the fact that the luminescent discharge acts on the cage wall instead of on the samples surface, which remains under a floating potential. In this work the enhancement of the cathodic cage nitriding layers proprieties, under several conditions for some types of steels was investigated, besides the mechanism for nitrides deposition on glass substrate, concluding that the CCPN is both a diffusion and a deposition process at the same time

Obtenção de álcool alílico (PROP-2-EN-1-OL) a partir da glicerina derivada do biodiesel de óleo de mamona

In this work, biodiesel was produced from castor oil that was a byproduct glycerin. The molar ratio between oil and alcohol, as well as the use of (KOH) catalyst to provide the chemical reaction is based on literature. The best results were obtained using 1 mol of castor oil (260g) to 3 moles of methyl alcohol (138g), using 1.0% KOH as catalyst at a temperature of 260 ° C and shaken at 120 rpm. The oil used was commercially available, the process involves the reaction of transesterification of a vegetable oil with methyl alcohol. The product of this reaction is an ester, biodiesel being the main product and the glycerin by-product which has undergone treatment for use as raw material for the production of allyl alcohol. The great advantage of the use of glycerin to obtain allyl alcohol is that its use eliminates the large amount of waste of the biodiesel and various forms of insult to the environment. The reactions for the formation of allyl alcohol was conducted from formic acid and glycerin in a ratio 1/1, at a temperature of 260oC in a heater blanket, being sprayed by a spiral condenser for a period of 2 hours and the product obtained contains mostly the allylic alcohol .. The monitoring of reactions was performed by UV-Visible Spectrophotometer: FTIR Fourier transform, the analysis showed that these changes occur spectrometer indicating the formation of the product allylic alcohol (prop-2-en-1-ol) in the presence of water, This alcohol was appointed Alcohol GL. The absorption bands confirms that the reaction was observed in (υ C = C) 1470 -1600 cm -1 and (υ CO), 3610-3670 attributed to C = C groups and OH respectively. The thermal analysis was carried out in a thermogravimetric analyzer SDT Q600, where the mass and temperature are displayed against time, that allows checking the approximate rate of heating. The innovative methodology developed in the laboratory (LABTAM, UFRN), was able to treat the glycerine produced by transesterification of castor oil and used as raw material for production of allyl alcohol, with a yield of 80%, of alcohol, the same is of great importance in the manufacture of polymers, pharmaceuticals, organic compounds, herbicides, pesticides and other chemicals

O renascimento do parto e da (reinvenção da) emancipação social na blogosfera brasileira: contra o desperdício das experiências

The birth models of care are discussed, in the light of classical and contemporary social science theoretical background, emphasizing the humanistic model. The double spiral of the sociology of absences and the sociology of emergences is detailed, being based, on one hand, on the translation of experiences of knowledge, and, on the other, on the translation of experiences of information and communication, by revealing the movement articulated by Brazilian women on blogs that defend and bring into light initiatives aiming to recover natural and humanized birth. A cartography of the thematic ideas in birth literature is produced, resulting in the elaboration of a synthetic map on obstetric models of care in contemporaneity, pointing out the consequences of the obstetric model that has become hegemonic in contemporary societies, and comparing that model to others that work more efficaciously to mothers and babies. A symbolic cartography of the activism for humanizing birth on the Brazilian blogosphere is configured by the elaboration of an analytical map synthetizing the main mottos defended by the movement: Normal humanized birth; Against obstetrical violence; and Planned home birth. The superposition of the obstetric models of care s map and the rebirth of birth s analytical map indicates it is necessary to reinforce three main measures in order to make a paradigmatic turn in contemporary birth models of care possible: pave the way for the humanistic care of assistance in normal birth, by defending and highlighting practices and professionals that act in compliance with evidence based medicine, respecting the physiology of birth; denaturalize obstetric violence, by showing how routine procedures and interventions can be means of aggression, jeopardizing the autonomy, the protagonism and the respect towards women; and motivate initiatives of planned home birth, the best place for the occurrence of holistic experiences of birth. It is concluded that Internet tools have allowed a pioneer mobilization in respecting women s reproductive rights in Brazil and that the potential of the crowd s biopower that resides on the blogosphere can turn blogs into a hegemonic alternative way to reach more democratic forms of social organization. In that condition of being virtually hegemonic in contesting the established power, these blogs can be understood, therefore, as potentially great contra-hegemonic channels for the rebirth of birth and for the reinvention of social emancipation, as their author s articulate and organize themselves to strive against the waste of experience, trying to create reciprocal intelligibility amongst different experiences of world

Para uma andragogia do esporte:discutindo as diretrizes e a formação profissional para a Educação Física de Jovens e Adultos

For the development of this research the following general objective has been formulated, indicator of the process of inquiry: To discuss the relation between the attitudinal and the sportive contents presented in the proposal of Curricular Lines for the Physical Education of Young and Adults in Brazil. According to the corporeity and the ludicity, questioning the formation of the professional of Physical Education and delineating the perspective for a sport andragogy that values the Being and the Life. From this general objective, the following objectives, which had given greater specificity to the investigative process, were defined: 1. To create the theoretical context from the corporeity/ludicity axis, articulating transversally sportive knowledge, aiming to contribute for a sport Andragogy; 2. To analyze the objectives proposed for the Physical Education of Young and Adults according to an elaborated theoretical reference and to the testimonies of the egresses of 2005 of the Physical Education course of the UFRN. 3. To interpret the relation between attitudinal and educative content from the academic reality lived by the egresses of the Physical Education course of the UFRN. 4. To understand the most urgent necessities of sustained formation of the egresses of 2005 for satisfactory performance with the Physical Education of Young and Adults. 5. To propose perspectives for the construction of a sport Andragogy from the corporeity/ludicity axis. In attendance to the nature of this research and as form of guiding ourselves in this epistemological adventure, the following ones had been basically and theoretically estimated. 1. Corporeity is a radiant focus, prime and main of educational criteria; 2. The task of the education must be carried through with men and not for men; 3. Man must only play with the beauty and with the beauty he only must play. ; 4. The sportive education must be based on esthetic and fair play. The adopted research approach is of a qualitative nature, using the interview procedure with a group consisting of twelve egresses of the Physical Education Course of the UFRN of the year of 2005.2 After the discussion of the results on the attitudinal objectives and content for the Physical Education for Adults and Young, the study shows nine themes presented by the investigated group as priorities for their sustained formation, aiming at the performance of the professional of Physical Education with the EJA: inclusive experiences; leisure and quality of life; relationships; body and personal care; social values; self esteem; sportive phenomenon; EJA training; attitudinal contents. As a contribution to the construction of knowledge for a Andragogy of Sports, the study presents a metaphorical structure called Galaxy of Knowledge righteous Glamor of integrating nine elements inspired by the Ode to the Sport of Pierre de Coubertin: life, beauty, justice, daring, honesty, joy; Fertility; progress; peace. At the heart of the structure of knowledge is righteous install a system that articulates five principles ludopoiético epistemological function of connecting with the righteous knowledge of the sport that must integrate the content attitudinal proposed for Fitness for Youth and Adults in order to facilitate the realization of their objectives proposed for this method of teaching

Estudo do acoplamento entre superfícies seletivas de frequência assimétricas em estruturas de multicamadas

This work presents the development of new microwaves structures, filters and high gain antenna, through the cascading of frequency selective surfaces, which uses fractals Dürer and Minkowski patches as elements, addition of an element obtained from the combination of the other two simple the cross dipole and the square spiral. Frequency selective surfaces (FSS) includes a large area of Telecommunications and have been widely used due to its low cost, low weight and ability to integrate with others microwaves circuits. They re especially important in several applications, such as airplane, antennas systems, radomes, rockets, missiles, etc. FSS applications in high frequency ranges have been investigated, as well as applications of cascading structures or multi-layer, and active FSS. In this work, we present results for simulated and measured transmission characteristics of cascaded structures (multilayer), aiming to investigate the behavior of the operation in terms of bandwidth, one of the major problems presented by frequency selective surfaces. Comparisons are made with simulated results, obtained using commercial software such as Ansoft DesignerTM v3 and measured results in the laboratory. Finally, some suggestions are presented for future works on this subject

Desenvolvimento de monopolos quase-espirais para aplicações em sistemas UWB

This work is the analysis of a structure of the microstrip antenna designed for application in ultra wide band systems (Ultra Wideband - UWB). This is a prospective analytical study where they tested the changes in the geometry of the antenna, observing their suitability to the proposed objectives. It is known that the UWB antenna must operate in a range of at least 500 MHz, and answer a fractional bandwidth greater than or equal to 25%. It is also desirable that the antenna meets the specifications of track determined by FCC - Federal Communication Commission, which regulates the system in 2002 designating the UWB bandwidth of 7.5 GHz, a range that varies from 3.1 GHz to 10, 6 GHz. by setting the maximum power spectral density of operation in -41.3 dB / MHz, and defining the fractional bandwidth by 20%. The study starts of a structure of geometry in the form of stylized @, which evolves through changes in its form, in simulated commercial software CST MICROWAVE STUDIO, version 5.3.1, and then tested using the ANSOFT HFSS, version 9. These variations, based on observations of publications available from literature referring to the microstrip monopole planar antennas. As a result it is proposed an antenna, called Monopole Antenna Planar Spiral Almost Rectangular for applications in UWB systems - AMQEUWB, which presents simulated and measured results satisfactory, consistent with the objectives of the study. Some proposals for future work are mentioned

Análise da eficiência de aquecedor solar espiral com e sem efeito estufa para piscinas

The technical and economic viability of solar heating for swimming pools is unquestionable, besides there it replaces the high costs and environmental impacts of conventional supply of energy, and it improves an optimization in the pool heating uses. This work applies the principles of the greenhouse effect: advanced thermodynamics, heat retention and equalization of temperature, to optimize the solar heating equipment, reducing the area required by collectors as much as 40% (still estimated value) for commercial collectors, with minor architectural and aesthetic impacts on the environment. It features a solar heating alternative in pools, whose main characteristics: low cost, simplicity in manufacturing and assembly and a faster heating. The system consists of two collectors spiral hoses made of polyethylene with a hundred meters each, and working on a forced flow, with only one pass of the working fluid inside the coils, and is used to pump itself treatment of pool water to obtain the desired flow. One of the collectors will be exposed to direct solar radiation, and the other will be covered by a glass slide and closed laterally, so providing the greenhouse effect. The equipment will be installed in parallel and simultaneously exposed to the sun in order to obtain comparative data on their effectiveness. Will be presented results of thermal tests for this the two cases, with and without transparent cover. Will be demonstrated, by comparison, the thermal, economic and material feasibility of these systems for heating swimming pools.

Acelaração do universo e criação gravitacional de matéria escura fria: novos modelos e testes observacionais

Recent astronomical observations (involving supernovae type Ia, cosmic background radiation anisotropy and galaxy clusters probes) have provided strong evidence that the observed universe is described by an accelerating, flat model whose space-time properties can be represented by the FriedmannRobertsonWalker (FRW) metric. However, the nature of the substance or mechanism behind the current cosmic acceleration remains unknown and its determination constitutes a challenging problem for modern cosmology. In the general relativistic description, an accelerat ing regime is usually obtained by assuming the existence of an exotic energy component endowed with negative pressure, called dark energy, which is usually represented by a cosmological constant ¤ associated to the vacuum energy density. All observational data available so far are in good agreement with the concordance cosmic ¤CDM model. Nevertheless, such models are plagued with several problems thereby inspiring many authors to propose alternative candidates in the relativistic context. In this thesis, a new kind of accelerating flat model with no dark energy and fully dominated by cold dark matter (CDM) is proposed. The number of CDM particles is not conserved and the present accelerating stage is a consequence of the negative pressure describing the irreversible process of gravitational particle creation. In order to have a transition from a decelerating to an accelerating regime at low redshifts, the matter creation rate proposed here depends on 2 parameters (y and ߯): the first one identifies a constant term of the order of H0 and the second one describes a time variation proportional to he Hubble parameter H(t). In this scenario, H0 does not need to be small in order to solve the age problem and the transition happens even if there is no matter creation during the radiation and part of the matter dominated phase (when the ß term is negligible). Like in flat ACDM scenarios, the dimming of distant type Ia supernovae can be fitted with just one free parameter, and the coincidence problem plaguing the models driven by the cosmological constant. ACDM is absent. The limits endowed with with the existence of the quasar APM 08279+5255, located at z = 3:91 and with an estimated ages between 2 and 3 Gyr are also investigated. In the simplest case (ß = 0), the model is compatible with the existence of the quasar for y > 0:56 whether the age of the quasar is 2.0 Gyr. For 3 Gyr the limit derived is y > 0:72. New limits for the formation redshift of the quasar are also established

Efeitos das inomogeneidades da matéria em Cosmologias Aceleradas

The recent observational advances of Astronomy and a more consistent theoretical framework turned Cosmology in one of the most exciting frontiers of contemporary science. In this thesis, homogeneous and inhomogeneous Universe models containing dark matter and different kinds of dark energy are confronted with recent observational data. Initially, we analyze constraints from the existence of old high redshift objects, Supernovas type Ia and the gas mass fraction of galaxy clusters for 2 distinct classes of homogeneous and isotropic models: decaying vacuum and X(z)CDM cosmologies. By considering the quasar APM 08279+5255 at z = 3.91 with age between 2-3 Gyr, we obtain 0,2 < OM < 0,4 while for the j3 parameter which quantifies the contribution of A( t) is restricted to the intervalO, 07 < j3 < 0,32 thereby implying that the minimal age of the Universe amounts to 13.4 Gyr. A lower limit to the quasar formation redshift (zJ > 5,11) was also obtained. Our analyzes including flat, closed and hyperbolic models show that there is no an age crisis for this kind of decaying A( t) scenario. Tests from SN e Ia and gas mass fraction data were realized for flat X(z)CDM models. For an equation of state, úJ(z) = úJo + úJIZ, the best fit is úJo = -1,25, úJl = 1,3 and OM = 0,26, whereas for models with úJ(z) = úJo+úJlz/(l+z), we obtainúJo = -1,4, úJl = 2,57 and OM = 0,26. In another line of development, we have discussed the influence of the observed inhomogeneities by considering the Zeldovich-Kantowski-DyerRoeder (ZKDR) angular diameter distance. By applying the statistical X2 method to a sample of angular diameter for compact radio sources, the best fit to the cosmological parameters for XCDM models are OM = O, 26,úJ = -1,03 and a = 0,9, where úJ and a are the equation of state and the smoothness parameters, respectively. Such results are compatible with a phantom energy component (úJ < -1). The possible bidimensional spaces associated to the plane (a , OM) were restricted by using data from SNe Ia and gas mass fraction of galaxy clusters. For Supernovas the parameters are restricted to the interval 0,32 < OM < 0,5(20") and 0,32 < a < 1,0(20"), while to the gas mass fraction we find 0,18 < OM < 0,32(20") with alI alIowed values of a. For a joint analysis involving Supernovas and gas mass fraction data we obtained 0,18 < OM < 0,38(20"). In general grounds, the present study suggests that the influence of the cosmological inhomogeneities in the matter distribution need to be considered with more detail in the analyses of the observational tests. Further, the analytical treatment based on the ZKDR distance may give non-negligible corrections to the so-calIed background tests of FRW type cosmologies

O enigmático problema das gigantes ricas em Lítio e as perspectivas com o satélite Kepler

Lithium (Li) is a chemical element with atomic number 3 and it is among the lightest known elements in the universe. In general, the Lithium is found in the nature under the form of two stable isotopes, the 6Li and 7Li. This last one is the most dominant and responds for about 93% of the Li found in the Universe. Due to its fragileness this element is largely used in the astrophysics, especially in what refers to the understanding of the physical process that has occurred since the Big Bang going through the evolution of the galaxies and stars. In the primordial nucleosynthesis in the Big Bang moment (BBN), the theoretical calculation forecasts a Li production along with all the light elements such as Deuterium and Beryllium. To the Li the BNB theory reviews a primordial abundance of Log log ǫ(Li) =2.72 dex in a logarithmic scale related to the H. The abundance of Li found on the poor metal stars, or pop II stars type, is called as being the abundance of Li primordial and is the measure as being log ǫ(Li) =2.27 dex. In the ISM (Interstellar medium), that reflects the current value, the abundance of Lithium is log ǫ(Li) = 3.2 dex. This value has great importance for our comprehension on the chemical evolution of the galaxy. The process responsible for the increasing of the primordial value present in the Li is not clearly understood until nowadays. In fact there is a real contribution of Li from the giant stars of little mass and this contribution needs to be well streamed if we want to understand our galaxy. The main objection in this logical sequence is the appearing of some giant stars with little mass of G and K spectral types which atmosphere is highly enriched with Li. Such elevated values are exactly the opposite of what could happen with the typical abundance of giant low mass stars, where convective envelops pass through a mass deepening in which all the Li should be diluted and present abundances around log ǫ(Li) ∼1.4 dex following the model of stellar evolution. In the Literature three suggestions are found that try to reconcile the values of the abundance of Li theoretical and observed in these rich in Li giants, but any of them bring conclusive answers. In the present work, we propose a qualitative study of the evolutionary state of the rich in Li stars in the literature along with the recent discovery of the first star rich in Li observed by the Kepler Satellite. The main objective of this work is to promote a solid discussion about the evolutionary state based on the characteristic obtained from the seismic analysis of the object observed by Kepler. We used evolutionary traces and simulation done with the population synthesis code TRILEGAL intending to evaluate as precisely as possible the evolutionary state of the internal structure of these groups of stars. The results indicate a very short characteristic time when compared to the evolutionary scale related to the enrichment of these stars