Constraining the orbital orientation of eta Carinae from H Paschen lines

During the past decade, several observational and theoretical works have provided evidence of the binary nature of eta Carinae. Nevertheless, there is still no direct determination of the orbital parameters, and the different current models give contradictory results. The orbit is, in general, assumed to coincide with the Homunculus equator although the observations are not conclusive. Among all systems, eta Car has the advantage that it is possible to observe both the direct emission of line transitions in the central source and its reflection by the Homunculus, which is dependent on the orbital inclination. In this work, we studied the orbital phase-dependent hydrogen Paschen spectra reflected by the south-east lobe of the Homunculus to constrain the orbital parameters of eta Car and determine its inclination with respect to the Homunculus axis. Assuming that the emission excess originates in the wind-wind shock region, we were able to model the latitude dependence of the spectral line profiles. For the first time, we were able to estimate the orbital inclination of eta Car with respect to the observer and to the Homunculus axis. The best fit occurs for an orbital inclination to the line of sight of i similar to 60 degrees +/- 10 degrees, and i* similar to 35 degrees +/- 10 degrees with respect to the Homunculus axis, indicating that the angular momenta of the central object and the orbit are not aligned. We were also able to fix the phase angle of conjunction as similar to -40 degrees, showing that periastron passage occurs shortly after conjunction.

SIMULATIONS OF WINDS OF WEAK-LINED T TAURI STARS: THE MAGNETIC FIELD GEOMETRY AND THE INFLUENCE OF THE WIND ON GIANT PLANET MIGRATION

By means of numerical simulations, we investigate magnetized stellar winds of pre-main-sequence stars. In particular, we analyze under which circumstances these stars will present elongated magnetic features (e.g., helmet streamers, slingshot prominences, etc). We focus on weak-lined T Tauri stars, as the presence of the tenuous accretion disk is not expected to have strong influence on the structure of the stellar wind. We show that the plasma-beta parameter (the ratio of thermal to magnetic energy densities) is a decisive factor in defining the magnetic configuration of the stellar wind. Using initial parameters within the observed range for these stars, we show that the coronal magnetic field configuration can vary between a dipole-like configuration and a configuration with strong collimated polar lines and closed streamers at the equator (multicomponent configuration for the magnetic field). We show that elongated magnetic features will only be present if the plasma-beta parameter at the coronal base is beta(0) << 1. Using our self-consistent three-dimensional magnetohydrodynamics model, we estimate for these stellar winds the timescale of planet migration due to drag forces exerted by the stellar wind on a hot-Jupiter. In contrast to the findings of Lovelace et al., who estimated such timescales using the Weber and Davis model, our model suggests that the stellar wind of these multicomponent coronae are not expected to have significant influence on hot-Jupiters migration. Further simulations are necessary to investigate this result under more intense surface magnetic field strengths (similar to 2-3 kG) and higher coronal base densities, as well as in a tilted stellar magnetosphere.

MODELING VERY LONG BASELINE INTERFEROMETRIC IMAGES WITH THE CROSS-ENTROPY GLOBAL OPTIMIZATION TECHNIQUE

We present a new technique for obtaining model fittings to very long baseline interferometric images of astrophysical jets. The method minimizes a performance function proportional to the sum of the squared difference between the model and observed images. The model image is constructed by summing N(s) elliptical Gaussian sources characterized by six parameters: two-dimensional peak position, peak intensity, eccentricity, amplitude, and orientation angle of the major axis. We present results for the fitting of two main benchmark jets: the first constructed from three individual Gaussian sources, the second formed by five Gaussian sources. Both jets were analyzed by our cross-entropy technique in finite and infinite signal-to-noise regimes, the background noise chosen to mimic that found in interferometric radio maps. Those images were constructed to simulate most of the conditions encountered in interferometric images of active galactic nuclei. We show that the cross-entropy technique is capable of recovering the parameters of the sources with a similar accuracy to that obtained from the very traditional Astronomical Image Processing System Package task IMFIT when the image is relatively simple (e. g., few components). For more complex interferometric maps, our method displays superior performance in recovering the parameters of the jet components. Our methodology is also able to show quantitatively the number of individual components present in an image. An additional application of the cross-entropy technique to a real image of a BL Lac object is shown and discussed. Our results indicate that our cross-entropy model-fitting technique must be used in situations involving the analysis of complex emission regions having more than three sources, even though it is substantially slower than current model-fitting tasks (at least 10,000 times slower for a single processor, depending on the number of sources to be optimized). As in the case of any model fitting performed in the image plane, caution is required in analyzing images constructed from a poorly sampled (u, v) plane.

CHANDRA AND SPITZER IMAGING OF THE INFRARED CLUSTER IN NGC 2071

We present results of a sensitive Chandra X-ray observation and Spitzer mid-infrared (mid-IR) observations of the IR cluster lying north of the NGC 2071 reflection nebula in the Orion B molecular cloud. We focus on the dense cluster core known as NGC 2071-IR, which contains at least nine IR sources within a 40 `` x 40 `` region. This region shows clear signs of active star formation including powerful molecular outflows, Herbig-Haro objects, and both OH and H(2)O masers. We use Spitzer Infrared Array Camera (IRAC) images to aid in X-ray source identification and to determine young stellar object (YSO) classes using mid-IR colors. Spitzer IRAC colors show that the luminous source IRS 1 is a class I protostar. IRS 1 is believed to be driving a powerful bipolar molecular outflow and may be an embedded B-type star or its progenitor. Its X-ray spectrum reveals a fluorescent Fe emission line at 6.4 keV, arising in cold material near the protostar. The line is present even in the absence of large flares, raising questions about the nature of the ionizing mechanism responsible for producing the 6.4 keV fluorescent line. Chandra also detects X-ray sources at or near the positions of IRS 2, IRS 3, IRS 4, and IRS 6 and a variable X-ray source coincident with the radio source VLA 1, located just 2 `` north of IRS 1. No IR data are yet available to determine a YSO classification for VLA 1, but its high X-ray absorption shows that it is even more deeply embedded than IRS 1, suggesting that it could be an even younger, less-evolved protostar.

THREE-DIMENSIONAL NUMERICAL SIMULATIONS OF MAGNETIZED WINDS OF SOLAR-LIKE STARS

By means of self-consistent three-dimensional magnetohydrodynamics (MHD) numerical simulations, we analyze magnetized solar-like stellar winds and their dependence on the plasma-beta parameter (the ratio between thermal and magnetic energy densities). This is the first study to perform such analysis solving the fully ideal three-dimensional MHD equations. We adopt in our simulations a heating parameter described by gamma, which is responsible for the thermal acceleration of the wind. We analyze winds with polar magnetic field intensities ranging from 1 to 20 G. We show that the wind structure presents characteristics that are similar to the solar coronal wind. The steady-state magnetic field topology for all cases is similar, presenting a configuration of helmet streamer-type, with zones of closed field lines and open field lines coexisting. Higher magnetic field intensities lead to faster and hotter winds. For the maximum magnetic intensity simulated of 20 G and solar coronal base density, the wind velocity reaches values of similar to 1000 km s(-1) at r similar to 20r(0) and a maximum temperature of similar to 6 x 10(6) K at r similar to 6r(0). The increase of the field intensity generates a larger ""dead zone"" in the wind, i.e., the closed loops that inhibit matter to escape from latitudes lower than similar to 45 degrees extend farther away from the star. The Lorentz force leads naturally to a latitude-dependent wind. We show that by increasing the density and maintaining B(0) = 20 G the system recover back to slower and cooler winds. For a fixed gamma, we show that the key parameter in determining the wind velocity profile is the beta-parameter at the coronal base. Therefore, there is a group of magnetized flows that would present the same terminal velocity despite its thermal and magnetic energy densities, as long as the plasma-beta parameter is the same. This degeneracy, however, can be removed if we compare other physical parameters of the wind, such as the mass-loss rate. We analyze the influence of gamma in our results and we show that it is also important in determining the wind structure.

ON THE NATURE OF THE PROTOTYPE LUMINOUS BLUE VARIABLE AG CARINAE. II. WITNESSING A MASSIVE STAR EVOLVING CLOSE TO THE EDDINGTON AND BISTABILITY LIMITS

We show that the significantly different effective temperatures (T(eff)) achieved by the luminous blue variable AG Carinae during the consecutive visual minima of 1985-1990 (T(eff) similar or equal to 22,800 K) and 2000-2001 (T(eff) similar or equal to 17,000 K) place the star on different sides of the bistability limit, which occurs in line-driven stellar winds around T(eff) similar to 21,000 K. Decisive evidence is provided by huge changes in the optical depth of the Lyman continuum in the inner wind as T(eff) changes during the S Dor cycle. These changes cause different Fe ionization structures in the inner wind. The bistability mechanism is also related to the different wind parameters during visual minima: the wind terminal velocity was 2-3 times higher and the mass-loss rate roughly two times smaller in 1985-1990 than in 2000-2003. We obtain a projected rotational velocity of 220 +/- 50 km s(-1) during 1985-1990 which, combined with the high luminosity (L(star) = 1.5 x 10(6) L(circle dot)), puts AG Car extremely close to the Eddington limit modified by rotation (Omega Gamma limit): for an inclination angle of 90 degrees, Gamma(Omega) greater than or similar to 1.0 for M(circle dot) less than or similar to 60. Based on evolutionary models and mass budget, we obtain an initial mass of similar to 100 M(circle dot) and a current mass of similar to 60-70 M(circle dot) for AG Car. Therefore, AG Car is close to, if not at, the Omega Gamma limit during visual minimum. Assuming M = 70 M(circle dot), we find that Gamma(Omega) decreases from 0.93 to 0.72 as AG Car expands toward visual maximum, suggesting that the star is not above the Eddington limit during maximum phases.

The evolution of the mass-metallicity relation in SDSS galaxies uncovered by astropaleontology

We have obtained the mass-metallicity (M-Z) relation at different lookback times for the same set of galaxies from the Sloan Digital Sky Survey, using the stellar metallicities estimated with our spectral synthesis code STARLIGHT. We have found that this relation steepens and spans a wider range in both mass and metallicity at higher redshifts. We have modelled the time evolution of stellar metallicity with a closed-box chemical evolution model, for galaxies of different types and masses. Our results suggest that the M-Z relation for galaxies with present-day stellar masses down to 10(10) M(circle dot) is mainly driven by the history of star formation and not by inflows or outflows.

Estudo experimental de microrreservatórios para controle do escoamento superficial

O crescimento desordenado das cidades tem gerado muitos problemas de infraestrutura e impactos ao meio ambiente. No que se refere aos recursos hídricos, problemas de abastecimento, poluição e enchentes são cada vez mais constantes. À medida que a cidade se urbaniza e se impermeabiliza, vários são os impactos que vão atuar no sentido de provocar ou agravar as enchentes urbanas. No caso da drenagem urbana é preciso repensar o que vem sendo feito, buscando soluções alternativas às atualmente apresentadas, uma vez que estas não têm se mostrado eficientes. Uma possível solução para estes problemas é a aplicação de medidas de controle do escoamento na fonte, dentre elas o microrreservatório de detenção. Baseando-se na busca de soluções para os problemas citados, este trabalho tem o objetivo geral de verificar experimentalmente o funcionamento de microrreservatórios de detenção no controle da geração do escoamento superficial. Para isso foi construído um módulo experimental nas dependências do IPH, composto por um microrreservatório de 1m3, monitorado através de linígrafos que registram as vazões de entrada e saída, recebendo contribuição de uma área de 337,5m2. O período de monitoramento iniciou em agosto de 2000 e se estendeu até janeiro de 2001. De posse dos dados coletados foi possível fazer uma análise da eficiência deste dispositivo no controle do escoamento superficial, bem como estudar a real necessidade de manutenção da estrutura. Também foi feita uma análise do impacto da presença de sedimentos (folhagens) na água de escoamento nas estruturas de descarga. O trabalho também deixa uma contribuição no que se refere a critérios de projeto e dimensionamento de estruturas desta natureza. Finalmente foi possível concluir que o sistema é eficiente no controle da vazão de pico, porém o reservatório não permitiu um aumento no tempo de resposta da bacia.

Growing research where economies grow: essays on strategy and international expansion of companies from emerging countries

In recent years, emerging countries have assumed an increasingly prominent position in the world economy, as growth has picked up in these countries and slowed in developed economies. Two related phenomena, among others, can be associated with this growth: emerging countries were less affected by the 2008-2009 global economic recession; and they increased their participation in foreign direct investment, both inflows and outflows. This doctoral dissertation contributes to research on firms from emerging countries through four independent papers. The first group of two papers examines firm strategy in recessionary moments and uses Brazil, one of the largest emerging countries, as setting for the investigation. Data were collected through a survey on Brazilian firms referring to the 2008-2009 global recession, and 17 hypotheses were tested using structural equation modeling based on partial least squares. Paper 1 offered an integrative model linking RBV to literatures on entrepreneurship, improvisation, and flexibility to indicate the characteristics and capabilities that allow a firm to have superior performance in recessions. We found that firms that pre-recession have a propensity to recognize opportunities and improvisation capabilities for fast and creative actions have superior performance in recessions. We also found that entrepreneurial orientation and flexibility have indirect effects. Paper 2 built on business cycle literature to study which strategies - pro-cyclical or counter-cyclical – enable superior performance in recessions. We found that while most firms pro-cyclically reduce costs and investments during recessions, a counter-cyclical strategy of investing in opportunities created by changes in the environment enables superior performance. Most successful are firms with a propensity to recognize opportunities, entrepreneurial orientation to invest, and flexibility to efficiently implement these investments. The second group of two papers investigated international expansion of multinational enterprises, particularly the use of distance for their location decisions. Paper 3 proposed a conceptual framework to examine circumstances under which distance is less important for international location decisions, taking the new perspective of economic institutional distance as theoretical foundation. The framework indicated that the general preference for low-distance countries is lower: (1) when the company is state owned, rather than private owned; (2) when its internationalization motives are asset, resource, or efficiency seeking, as opposed to market seeking; and (3) when internationalization occurred after globalization and the advent of new technologies. Paper 4 compared five concurrent perspectives of distance and indicated their suitability to the study of various issues based on industry, ownership, and type, motive, and timing of internationalization. The paper also proposed that distance represents the disadvantages of host countries for international location decisions; as such, it should be used in conjunction with factors that represent host country attractiveness, or advantages as international locations. In conjunction, papers 3 and 4 provided additional, alternative explanations for the mixed empirical results of current research on distance. Moreover, the studies shed light into the discussion of differences between multinational enterprises from emerging countries versus those from advanced countries.

Economic recovery from the Argentine great depression : institutions, expectations, and the change of macroeconomic regime

This work explores how Argentina overcame the Great Depression and asks whether active macroeconomic interventions made any contribution to the recovery. In particular, we study Argentine macroeconomic policy as it deviated from gold-standard orthodoxy after the final suspension of convertibility in 1929. As elsewhere, fiscal policy in Argentina was conservative, and had little power to smooth output. Monetary policy became heterodox after 1929. The first and most important stage of institutional change took place with the switch from a metallic monetary regime to a fiduciary regime in 1931; the Caja de Conversión (Conversion Office, a currency board) began rediscounting as a means to sterilize gold outflows and avoid deflationary pressures, thus breaking from orthodox "mIes of the game." However, the actual injections of liquidity were small' and were not enough to fully offset the incipient monetary contractions: the "Keynes" effect was weak or negative. Rather, recovery derived from changes in beliefs and expectations surrounding the shift in the monetary and exchange-rate regime,and the delinking of gold flows and the money base. Agents perceivod a new regime, as shown by the path of consumption, investment, and estimated ex ante real interest rates: the "Mundell" effect was dominant. Notably, this change of regime predated a later, and supposedly more significant, stage of institutional reform, namely the creation of the central bank in 1935. Still, the extent of intervention was weak, and insufficient to fully offset externaI shocks to prices and money. Argentine macropolicy was heterodox in terms of the change of regime, but still conservative in terms of the tentative scope of the measures taken .

Are returns on Foreign Direct Investment (FDI), FDI determinants?

Foreign Direct Investments (FDI) acquired an important role in the development process of the global economy. FDI inward stock was equivalent to an average of 32% of GDP for OECD countries in 2013. However, FDI affects a country’s Balance of Payments (BoP) in two ways: FDI flows are recorded in the BoP financial account while returns on FDI affect the BoP current account. Therefore, part of the positive contribution of inward FDI to a country on its financial account could be potentially offset by a negative contribution of FDI returns on the current account. The intent of this work is to complement the research on FDI determinants by introducing FDI returns as a variable in a gravity model where bilateral FDI outflows are the dependent variable. Moreover, using outward FDI flows as the dependent variable, the work allows looking at the behavior of Multinational Corporations (MNC) investing abroad. The results show that MNCs repatriate returns generating from the investments they make abroad. This is particularly true when high-income countries are involved: MNCs from high-income countries repatriate returns to their home countries from FDI made anywhere, while MNCs from middle-income countries repatriate returns from FDI in high-income countries. Repatriated returns are a relevant variable determining the value of FDI that a country makes in another country. The information on FDI returns is starting to become available to the public. This allows MNCs to sharpen their investment location decision models and national IPAs to better assess the two-fold BoP effects of promoting FDI.

Eficiência de um hidrociclone de geometria rietema para pré-filtragem de água para irrigação

O hidrociclone é um equipamento amplamente utilizado pela indústria em processos envolvendo separação sólido-líquido, porém ainda pouco utilizado na agricultura irrigada no Brasil. Neste trabalho, avaliou-se o desempenho deste equipamento como pré-filtrante de partículas sólidas, oriundas dos processos erosivos e do assoreamento dos recursos hídricos. Os testes foram realizados com um hidrociclone de geometria Rietema, possuindo diâmetro de 19,2 cm na parte cilíndrica, operando com vazões variando entre 10 m³ h-1 e 27 m³ h-1. Os materiais particulados usados em suspensão foram: solo franco-argiloso e areia de rio. Os resultados mostraram que a perda de carga máxima média foi de 52 kPa e 47 kPa para as suspensões aquosas de areia e solo, respectivamente. Seu melhor desempenho ocorreu operando com suspensão aquosa de areia, apresentando eficiência total de 92,3% para a vazão de 26,9 m³ h-1. Concluiu-se que o equipamento avaliado é mais eficiente para remoção de partículas de areia, podendo ser utilizado como pré-filtro em sistemas de irrigação.

Abertura comercial, internacionalização e competitividade: a indústria brasileira de máquinas têxteis após os anos 1990

Este artigo avalia os resultados do processo de reestruturação da indústria brasileira de máquinas têxteis, originado pelas reformas econômicas liberalizantes iniciadas no final dos anos 1980 e início dos 1990 e pelas medidas macroeconômicas que deram sustentação ao Plano Real, a partir de julho de 1994. Inicialmente, fazemos uma avaliação teórica das fontes do conhecimento e das formas de capacitação tecnológica nessa indústria. A seguir, expomos brevemente as principais características da indústria de máquinas têxteis em âmbito global. Posteriormente, direcionando a discussão para o caso brasileiro, apresentamos as especificidades da indústria têxtil, usuária daqueles bens, e do próprio setor de máquinas nacional. Através dos fluxos de comércio exterior do Brasil entre 1990 e 2004 e da variação do valor médio (US$ FOB/KG) desses fluxos, o artigo examina as mudanças estruturais, tecnológicas e, por conseguinte, na competitividade, que culminaram na transformação da indústria brasileira de máquinas têxteis, em termos de dimensão (escala) e escopo, e em uma nova inserção internacional, agora mais especializada e subordinada.

Foreign Investment in Latin America and the Caribbean 2003

Includes bibliography

Foreign Investment in Latin America and the Caribbean 2006

Includes bibliography