Suppression of small baryonic structures due to a primordial magnetic field

We investigate the impact of the existence of a primordial magnetic field on the filter mass, characterizing the minimum baryonic mass that can form in dark matter (DM) haloes. For masses below the filter mass, the baryon content of DM haloes are severely depressed. The filter mass is the mass when the baryon to DM mass ratio in a halo is equal to half the baryon to DM ratio of the Universe. The filter mass has previously been used in semi-analytic calculations of galaxy formation, without taking into account the possible existence of a primordial magnetic field. We examine here its effect on the filter mass. For homogeneous comoving primordial magnetic fields of B(0) similar to 1 or 2 nG and a re-ionization epoch that starts at a redshift z(s) = 11 and is completed at z(r) = 8, the filter mass is increased at redshift 8, for example, by factors of 4.1 and 19.8, respectively. The dependence of the filter mass on the parameters describing the re-ionization epoch is investigated. Our results are particularly important for the formation of low-mass galaxies in the presence of a homogeneous primordial magnetic field. For example, for B(0) similar to 1 nG and a re-ionization epoch of z(s) similar to 11 and z(r) similar to 7, our results indicate that galaxies of total mass M similar to 5 x 108 M(circle dot) need to form at redshifts z(F) greater than or similar to 2.0, and galaxies of total mass M similar to 108 M(circle dot) at redshifts z(F) greater than or similar to 7.7.

VISTA Variables in the Via Lactea (VVV): The public ESO near-IR variability survey of the Milky Way

We describe the public ESO near-IR variability survey (VVV) scanning the Milky Way bulge and an adjacent section of the mid-plane where star formation activity is high. The survey will take 1929 h of observations with the 4-m VISTA telescope during 5 years (2010-2014), covering similar to 10(9) point sources across an area of 520 deg(2), including 33 known globular clusters and similar to 350 open clusters. The final product will be a deep near-IR atlas in five passbands (0.9-2.5 mu m) and a catalogue of more than 106 variable point sources. Unlike single-epoch surveys that, in most cases, only produce 2-D maps, the VVV variable star survey will enable the construction of a 3-D map of the surveyed region using well-understood distance indicators such as RR Lyrae stars, and Cepheids. It will yield important information on the ages of the populations. The observations will be combined with data from MACHO, OGLE, EROS, VST, Spitzer, HST, Chandra, INTEGRAL, WISE, Fermi LAT, XMM-Newton, GAIA and ALMA for a complete understanding of the variable sources in the inner Milky Way. This public survey will provide data available to the whole community and therefore will enable further studies of the history of the Milky Way, its globular cluster evolution, and the population census of the Galactic Bulge and center, as well as the investigations of the star forming regions in the disk. The combined variable star catalogues will have important implications for theoretical investigations of pulsation properties of stars. (C) 2009 Elsevier B.V. All rights reserved.

An accelerating cosmology without dark energy

The negative pressure accompanying gravitationally-induced particle creation can lead to a cold dark matter (CDM) dominated, accelerating Universe (Lima et al. 1996 [1]) without requiring the presence of dark energy or a cosmological constant. In a recent study, Lima et al. 2008 [2] (LSS) demonstrated that particle creation driven cosmological models are capable of accounting for the SNIa observations [3] of the recent transition from a decelerating to an accelerating Universe, without the need for Dark Energy. Here we consider a class of such models where the particle creation rate is assumed to be of the form Gamma = beta H + gamma H(0), where H is the Hubble parameter and H(0) is its present value. The evolution of such models is tested at low redshift by the latest SNe Ia data provided by the Union compilation [4] and at high redshift using the value of z(eq), the redshift of the epoch of matter - radiation equality, inferred from the WMAP constraints on the early Integrated Sachs-Wolfe (ISW) effect [5]. Since the contributions of baryons and radiation were ignored in the work of LSS, we include them in our study of this class of models. The parameters of these more realistic models with continuous creation of CDM are constrained at widely-separated epochs (z(eq) approximate to 3000 and z approximate to 0) in the evolution of the Universe. The comparison of the parameter values, {beta, gamma}, determined at these different epochs reveals a tension between the values favored by the high redshift CMB constraint on z(eq) from the ISW and those which follow from the low redshift SNIa data, posing a potential challenge to this class of models. While for beta = 0 this conflict is only at less than or similar to 2 sigma, it worsens as beta increases from zero.

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.

Desbaste da limeira-ácida-'Tahiti' (Citrus latifolia Tanaka) com TPA e efeitos na produção

Foram avaliadas concentrações de 0; 10; 20; 40 e 80 mg/L do 3,5,6-TPA (Ácid 3,5,6-tricloro-2-piridil- oxiacético), em sua formulação éster, para desbaste de frutos novos da limeira-ácida-'Tahiti' (Citrus latifolia Tanaka), nas condições ecológicas do Estado de São Paulo. O 3,5,6-TPA, na concentração 10mg/L, foi o tratamento mais eficaz para uso na cultura. Concentrações maiores causaram severos danos às plantas. Essa concentração, aplicada logo após a florada de outubro, reduziu em 65% a produção do mês de fevereiro seguinte. Todavia, as produções dos meses subseqüentes não diferiram entre si. A concentração de 10mg/L causou alongamento dos frutos, aumento da espessura da casca e redução do Brix, na época da colheita.

O púlpito como cátedra: retórica e educação nos sermões do Pe. Antônio Vieira (1608-1697)

This work aims to analyze the relationship among culture, education and rhetoric on the sermons of the Priest Antonio Vieira (1608-1697). It discusses the presence of oratory on the Western teaching since its Greek origins until the formation of the Ratio Studiorum in 17th-century. Brazilian society is defined as baroque and the rhetoric arises as element essential in the elaboration of the social imaginary speeches and, occupying as an essencial element in the elaboration of discursese and social imaginaries, occupying the centre of controversies, about questions like reason and the faith, ethics and the politics, the nature of the Indian and African peoples, even over the own construction of the modern subject. In this context the vieira´s preaching discharges the functions of kerigma (preaching), didachê (education) and politics (action). The research consisted in a finicky reading over five of these sermons that were returned in the presence of different audiences. The pulpit was the cathedra where Vieira used his sermons as a manner of social mobilization that aimed not only teaching a determined knowledge of reality, but altering cruel situations like Indian and poor people slavery in his epoch. Education by Vieira consist in a tension between utopian hopes and urgencies of practice. The rhetorical tradition affirms the interdependence of technical ethics and politics aspects. To know is not enough is necessary to convince and to move, realizating passage from theorical to practical liverly. It presupposes still the preoccupation with the solidity of argumentation and of reasoning, a wide cultural formation, the requirement of a civic ethics and, mainly, the adequacy between content and the specifics of audience

Propagação vegetativa de porta-enxertos para citros

O enraizamento de estacas é um método de propagação assexuada que mantém as características da planta-mãe e incrementa o número de plantas rapidamente, o que é de grande interesse para a citricultura, além de permitir a propagação de materiais na fase juvenil. A obtenção de porta-enxertos por estaquia é uma prática que pode possibilitar, além da redução do prazo na formação da muda, produção de plantas de menor porte e garantir a uniformidade do pomar. O objetivo do presente trabalho consistiu na observação e comparação da propagação vegetativa, por enraizamento de estacas, de quatro porta-enxertos utilizados na produção de mudas cítricas (Poncirus trifoliata, Citrus volkameriana, Citrumelo Swingle e Citrus limonia), sob a influência de diferentes doses de IBA (ácido indolbutírico). O experimento foi conduzido em câmara de nebulização intermitente, e as estacas foram imersas em soluções com 0; 100; 200 e 400 mg.L-1 de IBA, por um período de 14 horas. Avaliaram-se: porcentagem de sobrevivência; porcentagem de enraizamento; comprimento, e número médios de raízes. Analisando os resultados, conclui-se que: o Citrus volkameriana e o Citrus limonia mostraram resultados superiores aos obtidos para as demais espécies estudadas; a porcentagem de sobrevivência é influenciada pela dose de IBA, pelo porta-enxerto e pela época de coleta das estacas; a porcentagem de enraizamento é influenciada pelas características genéticas do porta-enxerto e época de coleta; o comprimento médio das raízes é influenciado pelo porta-enxerto e época de coleta das estacas; o número médio de raízes é influenciado pela dose de IBA e pelo porta-enxerto.

Propagação vegetativa de aroeira-pimenteira (Schinus terebinthifolius Raddi)

Este trabalho foi realizado com o objetivo de avaliar os melhores métodos e épocas de realização da enxertia, sobre o pegamento de enxertos de aroeira-pimenteira (Schinus terebinthifolius Raddi). Foram conduzidos dois experimentos, instalados na Faculdade de Ciências Agronômicas, da Universidade Estadual Paulista - Câmpus de Botucatu-SP, nos períodos de 16 de dezembro de 2005 a 30 de janeiro 2006 e de 03 de junho a 17 de julho de 2006. O delineamento utilizado foi de blocos casualizados, com cinco tratamentos, três repetições cada e dez plantas por parcela. Os tratamentos foram: garfagem no topo em fenda cheia, inglês simples, inglês complicado; borbulhia em T normal e T invertido. As diferentes épocas do ano alteraram o índice de pegamento, o que restringe o período de coleta de garfos. A maior porcentagem de pegamento ocorreu no mês de dezembro, com a enxertia em fenda cheia (40%). No mês de junho, não houve pegamento significativo, mostrando então que o mês de dezembro é o mês ideal, entre os estudados, para a realização da enxertia em aroeira. As garfagens em geral foram superiores à borbulhia. Houve baixo índice de pegamento, quando não foi nulo, e, além disso, suas borbulhas não apresentaram brotos dentro de 45 dias. A maior porcentagem de plantas com brotos, aos 45 dias, foi pelo método inglês simples, com 92%.

Integration of a regional GPS network within ITRF using precise point positioning

GPS precise point positioning (PPP) can provide high precision 3-D coordinates. Combined pseudorange and carrier phase observables, precise ephemeris and satellite clock corrections, together with data from dual frequency receivers, are the key factors for providing such levels of precision (few centimeters). In general, results obtained from PPP are referenced to an arbitrary reference frame, realized from a previous free network adjustment, in which satellite state vectors, station coordinates and other biases are estimated together. In order to obtain consistent results, the coordinates have to be transformed to the relevant reference frame and the appropriate daily transformation parameters must be available. Furthermore, the coordinates have to be mapped to a chosen reference epoch. If a velocity field is not available, an appropriated model, such as NNR-NUVEL-IA, has to be used. The quality of the results provided by this approach was evaluated using data from the Brazilian Network for Continuous Monitoring of the Global Positioning System (RBMC), which was processed using GIPSY-OASIS 11 software. The results obtained were compared to SIRGAS 1995.4 and ITRF2000, and reached precision better than 2cm. A description of the fundamentals of the PPP approach and its application in the integration of regional GPS networks with ITRF is the main purpose of this paper.

Stochastic modelling considering ionospheric scintillation effects on GNSS relative and point positioning

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Improving the GNSS positioning stochastic model in the presence of ionospheric scintillation

Ionospheric scintillations are caused by time-varying electron density irregularities in the ionosphere, occurring more often at equatorial and high latitudes. This paper focuses exclusively on experiments undertaken in Europe, at geographic latitudes between similar to 50 degrees N and similar to 80 degrees N, where a network of GPS receivers capable of monitoring Total Electron Content and ionospheric scintillation parameters was deployed. The widely used ionospheric scintillation indices S4 and sigma(phi) represent a practical measure of the intensity of amplitude and phase scintillation affecting GNSS receivers. However, they do not provide sufficient information regarding the actual tracking errors that degrade GNSS receiver performance. Suitable receiver tracking models, sensitive to ionospheric scintillation, allow the computation of the variance of the output error of the receiver PLL (Phase Locked Loop) and DLL (Delay Locked Loop), which expresses the quality of the range measurements used by the receiver to calculate user position. The ability of such models of incorporating phase and amplitude scintillation effects into the variance of these tracking errors underpins our proposed method of applying relative weights to measurements from different satellites. That gives the least squares stochastic model used for position computation a more realistic representation, vis-a-vis the otherwise 'equal weights' model. For pseudorange processing, relative weights were computed, so that a 'scintillation-mitigated' solution could be performed and compared to the (non-mitigated) 'equal weights' solution. An improvement between 17 and 38% in height accuracy was achieved when an epoch by epoch differential solution was computed over baselines ranging from 1 to 750 km. The method was then compared with alternative approaches that can be used to improve the least squares stochastic model such as weighting according to satellite elevation angle and by the inverse of the square of the standard deviation of the code/carrier divergence (sigma CCDiv). The influence of multipath effects on the proposed mitigation approach is also discussed. With the use of high rate scintillation data in addition to the scintillation indices a carrier phase based mitigated solution was also implemented and compared with the conventional solution. During a period of occurrence of high phase scintillation it was observed that problems related to ambiguity resolution can be reduced by the use of the proposed mitigated solution.

Uma leitura dos exercícios dos excursos n Os Lusíadas

The Lusiads is an epic poem, written by Luís de Camões, about the adventure of Vasco da Gama s trip and the history of Portugal. It's based on traditionals epics from the Greek and Roman poets, Homero and Virgílio. Camões followes especially their structures. However, the poet insert modifications that divert his poem from parameters established by Aristóteles for the classic epic poems. These deviations are centered mainly on the narrative subject and in the point of view. We intend to show an analysis focused on digressions from The Lusiads, in which the author, himself or by tellers characters, narrates the story in order to make his complaints, reflections and exhortations. Besides, we present general aspects of Maneirismo predominant in these digressions how evidences of modernity of the poem; as one brief outlook about the poem's projection in time and around the world. These points are importants elements of consolidation of a universal permanence of The Lusiads. That's why they have had to read and to study by the centuries, according the vision of the epoch's spirit

Criação da matéria em cosmologias com velocidade da luz variável e eletrônico não-linear

In this work we obtain the cosmological solutions and investigate the thermodynamics of matter creation in two diferent contexts. In the first we propose a cosmological model with a time varying speed of light c. We consider two diferent time dependence of c for a at Friedmann-Robertson- Walker (FRW) universe. We write the energy conservation law arising from Einstein equations and study how particles are created as c decreases with cosmic epoch. The variation of c is coupled to a cosmological Λ term and both singular and non-singular solutions are possible. We calculate the "adiabatic" particle creation rate and the total number of particles as a function of time and find the constrains imposed by the second law of thermodynamics upon the models. In the second scenario, we study the nonlinearity of the electrodynamics as a source of matter creation in the cosmological models with at FRW geometry. We write the energy conservation law arising from Einstein field equations with cosmological term Λ, solve the field equations and study how particles are created as the magnetic field B changes with cosmic epoch. We obtain solutions for the adiabatic particle creation rate, the total number of particles and the scale factor as a function of time in three cases: Λ = 0, Λ = constant and Λ α H2 (cosmological term proportional to the Hubble parameter). In all cases, the second law of thermodynamics demands that the universe is not contracting (H ≥ 0). The first two solutions are non-singular and exhibit in ationary periods. The third case studied allows an always in ationary universe for a suficiently large cosmological term

Evolução de estruturas primordiais

Understanding the way in which large-scale structures, like galaxies, form remains one of the most challenging problems in cosmology today. The standard theory for the origin of these structures is that they grew by gravitational instability from small, perhaps quantum generated, °uctuations in the density of dark matter, baryons and photons over an uniform primordial Universe. After the recombination, the baryons began to fall into the pre-existing gravitational potential wells of the dark matter. In this dissertation a study is initially made of the primordial recombination era, the epoch of the formation of the neutral hydrogen atoms. Besides, we analyzed the evolution of the density contrast (of baryonic and dark matter), in clouds of dark matter with masses among 104M¯ ¡ 1010M¯. In particular, we take into account the several physical mechanisms that act in the baryonic component, during and after the recombination era. The analysis of the formation of these primordial objects was made in the context of three models of dark energy as background: Quintessence, ¤CDM(Cosmological Constant plus Cold Dark Matter) and Phantom. We show that the dark matter is the fundamental agent for the formation of the structures observed today. The dark energy has great importance at that epoch of its formation

Bounds on direct couplings of superheavy metastable particles to the inflaton field from ultra high energy cosmic ray events

Top-down models for the origin of ultra high energy cosmic rays (UHECR's) propose that these events are the decay products of relic superheavy metastable particles, usually called X particles. These particles can be produced in the reheating period following the inflationary epoch of the early Universe. We obtain constraints on some parameters such as the lifetime and direct couplings of the X-particle to the inflaton field from the requirement that they are responsible for the observed UHECR flux.