TOWARD UNDERSTANDING THE B[e] PHENOMENON. IV. MODELING OF IRAS 00470+6429

FS CMa type stars are a recently described group of objects with the B[e] phenomenon which exhibits strong emission-line spectra and strong IR excesses. In this paper, we report the first attempt for a detailed modeling of IRAS 00470+6429, for which we have the best set of observations. Our modeling is based on two key assumptions: the star has a main-sequence luminosity for its spectral type (B2) and the circumstellar (CS) envelope is bimodal, composed of a slowly outflowing disklike wind and a fast polar wind. Both outflows are assumed to be purely radial. We adopt a novel approach to describe the dust formation site in the wind that employs timescale arguments for grain condensation and a self-consistent solution for the dust destruction surface. With the above assumptions we were able to satisfactorily reproduce many observational properties of IRAS 00470+6429, including the Hi line profiles and the overall shape of the spectral energy distribution. Our adopted recipe for dust formation proved successful in reproducing the correct amount of dust formed in the CS envelope. Possible shortcomings of our model, as well as suggestions for future improvements, are discussed.

Open cluster survival within the solar circle: Teutsch 145 and Teutsch 146 star

Teutsch 145 and Teutsch 146 are shown to be open clusters (OCs) orbiting well inside the solar circle, a region where several dynamical processes combine to disrupt most OCs on a time-scale of a few 108 yr. BVI photometry from the GALILEO telescope is used to investigate the nature and derive the fundamental and structural parameters of the optically faint and poorly known OCs Teutsch 145 and 146. These parameters are computed by means of field-star-decontaminated colour-magnitude diagrams and stellar radial density profiles (RDPs). Cluster mass estimates are made based on the intrinsic mass functions (MFs). We derive the ages 200+100(-50) and 400 +/- 100 Myr, and the distances from the Sun d(circle dot) = 2.7 +/- 0.3 and 3.8 +/- 0.2 kpc, respectively, for Teutsch 145 and 146. Their integrated apparent and absolute magnitudes are m(V) approximate to 12.4 and 13.3 and M(V) approximate to -5.6 and -5.3. The MFs (detected for stars with m greater than or similar to 1 M(circle dot)) have slopes similar to Salpeter`s initial mass function. Extrapolated to the H-burning limit, the MFs would produce total stellar masses of similar to 1400 M(circle dot), typical of relatively massive OCs. Both OCs are located deep into the inner Galaxy and close to the Crux-Scutum arm. Since cluster-disruption processes are important, their primordial masses must have been higher than the present-day values. The conspicuous stellar density excess observed in the innermost bin of both RDPs might reflect the dynamical effects induced by a few 108 yr of external tidal stress.

Further probing the nature of FSR 1767

With Two-Micron All-Sky Survey (2MASS) photometry and proper motions, Bonatto et al. suggested that FSR 1767 is a globular cluster (GC), while with J and K NTT/SOFI photometry Froebrich, Meusinger & Scholz concluded that it is not a star cluster. In this study, we combine previous and new evidence that are consistent with a GC. For instance, we show that the horizontal branch (HB) and red giant branch (RGB) stars, besides sharing a common proper motion, have radial density profiles that consistently follow the King`s law independently. Reddening maps around FSR 1767 are built using the bulge RGB as reference and also Schlegel`s extinction values to study local absorptions. Both approaches provide similar maps and show that FSR 1767 is not located in a dust window, which otherwise might have produced the stellar overdensity. Besides, neighbouring regions of similar reddening as FSR 1767 do not present the blue HB stars that are a conspicuous feature in the colour-magnitude diagram of FSR 1767. We report the presence of a compact group of stars located in the central parts of FSR 1767. It appears to be a detached post-collapse core, similar to those of other nearby low-luminosity GCs projected towards the bulge. We note that while the NTT/SOFI photometry of the star cluster FSR 1716 matches perfectly that from 2MASS, it shows a considerable offset for FSR 1767. We discuss the possible reasons why both photometries differ. We confirm our previous structural and photometric fundamental parameters for FSR 1767, which are consistent with a GC.

TOWARD UNDERSTANDING THE B[e] PHENOMENON. III. PROPERTIES OF THE OPTICAL COUNTERPART OF IRAS 00470+6429

FS CMa type stars are a group of Galactic objects with the B[e] phenomenon. They exhibit strong emission-line spectra and infrared excesses, which are most likely due to recently formed circumstellar dust. The group content and identification criteria were described in the first two papers of the series. In this paper we report our spectroscopic and photometric observations of the optical counterpart of IRAS 00470+6429 obtained in 2003-2008. The optical spectrum is dominated by emission lines, most of which have P Cyg type profiles. We detected significant brightness variations, which may include a regular component, and variable spectral line profiles in both shape and position. The presence of a weak Li I 6708 angstrom line in the spectrum suggests that the object is most likely a binary system with a B2-B3 spectral-type primary companion of a luminosity log L/L(circle dot) = 3.9 +/- 0.3 and a late-type secondary companion. We estimate a distance toward the object to be 2.0 +/- 0.3 kpc from the Sun.

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 influence of halo assembly on galaxies and galaxy groups

In this paper, we study the variations of groups (galaxy properties according to the assembly history in Sloan Digital Sky Survey Data Release 6 (SDSS-DR6) selected groups. Using mock SDSS group catalogues, we find two suitable indicators of group formation time: (i) the isolation of the group, defined as the distance to the nearest neighbour ill terms of its virial radius and 00 the concentration. measured as the groups inner density calculated using the fifth nearest bright galaxy to the groups centre. Groups Within narrow ranges of Mass ill the mock catalO-Lie show increasing Ifl-OLIP alle With isolation and concentration. However, in the observational data the stellar age, as indicated by the spectral type, only shows a correlation with concentration. We study groups of similar mass and different assembly history. finding important differences ill their galaxy population. Particularly, ill high-mass SDSS groups. the number of members. mass-to-light ratios, red galaxy fractions and the magnitude difference between the brightest and second-brightest group galaxies, show different trends as a function of isolation and concentration, even when it is expected that the latter two quantities correlate with group age. Conversely. low-mass SDSS groups appear to be less sensitive to their assembly history. The correlations detected in the SDSS are not consistent with the trends measured in the mock catalogues. However, discrepancies can he explained in terms of the disagreement found in the a-e-isolation trends, suggesting that the model might be overestimating the effects of, environment, We discuss how the modelling of the cold gas ill satellite galaxies could be responsible for this problem. These results call be Used to improve our Understanding of the evolution of galaxies ill high-density environments.

A faraway quasar in the direction of the highest energy Auger event

The highest energy cosmic ray event reported by the Auger Observatory has an energy of 148 EeV. It does not correlate with any nearby (z<0.024) object capable of originating such a high energy event. Intrigued by the fact that the highest energy event ever recorded (by the Fly`s Eye collaboration) points to a faraway quasar with very high radio luminosity and large Faraday rotation measurement, we have searched for a similar source for the Auger event. We find that the Auger highest energy event points to a quasar with similar characteristics to the one correlated to the Fly`s Eye event. We also find the same kind of correlation for one of the highest energy AGASA events. We conclude that so far these types of quasars are the best source candidates for both Auger and Fly`s Eye highest energy events. We discuss a few exotic candidates that could reach us from gigaparsec distances.

Scrutinizing the ZW(+)W(-) vertex at the Large Hadron Collider at 7 TeV

We analyze the potential of the CERN Large Hadron Collider running at 7 TeV to search for deviations from the Standard Model predictions for the triple gauge boson coupling ZW(+)W(-) assuming an integrated luminosity of 1 fb(-1). We show that the study of W(+)W(-) and W(+/-)Z productions, followed by the leptonic decay of the weak gauge bosons can improve the present sensitivity on the anomalous couplings Delta g(1)(Z), Delta kappa(Z), lambda(Z), g(4)(Z), and (lambda) over bar (Z) at the 2 sigma level. (C) 2010 Elsevier B.V. All rights reserved.

Links hipertextuais na comunicação científica: análise webométrica dos sítios acadêmicos latino-americanos em ciências sociais

VANTI, Nadia. Links hipertextuais na comunicação científica: análise webométrica dos sítios acadêmicos latino-americanos em Ciências Sociais. Porto Alegre, 2007. 292 f. Tese (Doutorado em Comunicação e Informação) – Universidade Federal do Rio Grande do Sul. Porto Alegre, 2007.

Mapeamento das Instituições Federais de Ensino Superior da Região Nordeste do Brasil na Web

VANTI, Nadia. Mapeamento das Instituições Federais de Ensino Superior da Região Nordeste do Brasil na Web. Informação & informação, Londrina, v. 15, p. 55-67, 2010

Efeitos de manipulações ascendentes e descendentes sobre a comunidade fitoplanctônica em um reservatório eutrófico no semi-árido brasileiro

Top-down (grazing) and bottom-up (nutrient, light) controls are important in freshwater ecosystems regulation. Relative importance of these factors could change in space and time, but in tropical lakes bottom-up regulation has to been appointed as more influent. Present study aimed to test the hypothesis that phytoplankton growths rate in Armando Ribeiro reservoir, a huge eutrophic reservoir in semi-arid region of Rio Grande do Norte state, is more limited by nutrient available then zooplankton grazing pressure. Bioassay was conduced monthly from September (2008) to August (2009) manipulating two levels of nutrients (with/without addition) and two level of grazers (with/without removal). Experimental design was factorial 2X2 with four treatments (X5), (i) control with water and zooplankton from natural spot ( C ), (ii) with nutrient addition ( +NP ), (iii) with zooplankton remove ( -Z ) and (iv) with zooplankton remove and nutrient addition ( -Z+NP ). For bioassay confection transparent plastic bottles (500ml) was incubate for 4 or 5 days in two different depths, Secchi`s depth (high luminosity) and 3 times Secchi`s depth (low luminosity). Water samples were collected from each bottle in begins and after incubates period for chlorophyll a concentration analysis and zoopalnktonic organisms density. Phytoplankton growths rates were calculated. Bifactorial ANOVA was performance to test if had a significant effect (p<0,005) of nutrient addition and grazers remove as well a significant interaction between factors on phytoplankton growths rates. Effect magnitude was calculated the relative importance of each process. Results show that phytoplankton growth was in generally stimulated by nutrient addition, as while zooplankton remove rarely stimulated phytoplankton growth. Some significant interactions happening between nutrient additions and grazers remove on phytoplankton growth. In conclusion this study suggests that in studied reservoir phytoplankton growth is more controlled by ascendent factors than descendent

Efeito da luz no crescimento de mudas de Hymenaea parvifolia Huber

Este trabalho teve como objetivo determinar o efeito da intensidade de luz no crescimento de mudas de Hymenaea parvifolia Huber., bem como inferir sobre o seu grau de tolerância à sombra. Para tal, foi instalado um experimento em delineamento inteiramente casualizado, com quatro tratamentos (níveis de luz): pleno sol (PS), 50% de sombreamento, 70% de sombreamento e sombreamento natural (SN). Os níveis de 50 e 70% de sombreamento foram obtidos com o uso de telas de polipropileno preto, e o sombreamento natural constituiu a luminosidade natural sob um dossel fechado de floresta. Cada tratamento foi constituído de 10 repetições. Plantas sob sombreamento (50% e 70% de sombreamento) apresentaram maior altura, área foliar e razão de área foliar e poucas diferenças no acúmulo de massa seca quando comparadas com plantas mantidas a pleno sol. Como conseqüência, poucas diferenças foram observadas na taxa de crescimento relativo das mudas desses tratamentos. Todavia, mudas mantidas sob sombreamento natural foram as que exibiram menor taxa de crescimento relativo e taxa assimilatória líquida. em conjunto, os resultados indicaram que Hymenaea parvifolia foi capaz de se ajustar para maximizar a aquisição de luz mesmo em condição muito limitante, como a proporcionada pelo sombreamento natural, e a produção de mudas dessa espécie vegetal pode ser realizada em viveiro desde a pleno sol, como a 50% ou 70% de sombreamento.

Características de qualidade da carne de ovinos de diferentes genótipos e idades ao abate

Cordeiros criados em regime de pasto, provenientes de ovelhas Romney acasaladas com três raças paternas (Romney, East Friesian x (Finn x Texel) e Finn x Poll Dorset), foram avaliados quanto às características de qualidade da carne. Os cordeiros foram abatidos aos 150 e 300 dias de idade, cada lote com 15 animais de cada raça paterna, totalizando 90 animais. A carne dos cordeiros Romney foi mais macia que a dos demais genótipos. O pH final do músculo Semimembranosus dos cordeiros abatidos mais precocemente foi superior (5,61) ao dos abatidos mais tardiamente (5,58), entretanto estes últimos apresentaram carne com menor maciez (11,16 kg) que os abatidos aos 150 dias de idade (7,45 kg). Com relação à cor, a luminosidade da carne de cordeiros abatidos aos 150 dias foi maior (38,20) que a dos abatidos mais tardiamente (36,80), mas não foi afetada pelo genótipo. Concluiu-se que o genótipo e a idade de abate influíram na produção e qualidade da carne ovina.

Caracterização de Diaporthe citri em diferentes meios de cultura, condições de temperatura e luminosidade

Estudou-se o crescimento micelial de dez isolados de Diaporthe citri, utilizando-se seis meios de cultura (aveia-ágar, maltose-peptona-ágar, batata-dextrose-ágar, folha de laranja-dextrose-ágar, folha de limão-dextrose-ágar, milho-ágar) à temperatura de 22 ± 2 °C e fotoperíodo de 12 h claro/12 h escuro. O cultivo em meio de batata-dextrose-ágar (BDA) foi conduzido em cinco temperaturas diferentes (10, 15, 20, 25 e 30 °C). Três diferentes regimes de luminosidade (12 h claro/12 h escuro, claro contínuo, escuro contínuo) foram utilizados para verificar o crescimento do fungo. Foram observadas variações na produção de picnídios e de massa micelial nos diferentes meios de cultura, temperaturas e regimes de luminosidade testados, sendo que, para a maioria dos isolados, o meio de cultura de aveia-ágar, a faixa de 20 a 25 °C e o regime de claro contínuo induziram maior crescimento micelial. A produção de picnídios foi maior para o regime de luz contínua. O teste de patogenicidade foi feito por inoculação de discos de micélio de 5 mm de diâmetro em ferimentos em ramos e caule de limão 'Feminelo' (Citrus limon) enxertado em citrumelo 'Swingle'(Poncirus trifoliolata x Citrus paradisi) e plantas de limão 'Cravo' (C. limonia) enxertados com laranja 'Valência' (C. sinensis). Após sete dias, houve o aparecimento de exsudação de goma nas plantas inoculadas com os isolados, mas não na testemunha. Todos os isolados mostraram-se patogênicos, sendo os isolados PC2 e PC5, os que causaram comprimento de lesão maior nas plantas.

Influência do alinhamento de plantio na severidade da mancha-preta-dos-citros, produção e qualidade do suco

Os níveis de incidência e severidade de sintomas das doenças resultam da interação hospedeiro-patógeno-ambiente. Nesse contexto, a favorabilidade do ambiente, em particular, depende do nível de umidade, intensidade de radiação solar, luminosidade e molhamento foliar, dentre outros fatores. Por outro lado, a magnitude de expressão desses fatores é dependente do ciclo e porte das plantas, e possivelmente, também, do alinhamento de plantio. No presente estudo, foi avaliada a influência dos alinhamentos de plantio N-S, L-O, NE-SO E NO-SE no desempenho agronômico de plantas de laranjas 'Natal'e 'Valência', assim como na severidade de sintomas da mancha-preta-dos-citros (MPC), causada por Guignardia citricarpa. Para tal, foram selecionadas cinco propriedades distribuídas ao longo do cinturão citrícola paulista, de talhões semelhantes, a partir das quais foram coletadas amostras de 50 frutos, em dez plantas de mesma linha, da região central dos mesmos. Tais frutos foram levados para laboratórios e analisados quanto aos níveis de severidade de sintomas da MPC, produção e qualidade do suco. Constatouse que os frutos oriundos de pomares implantados no alinhamento N-S apresentavam menores níveis de severidade da doença, enquanto no alinhamento NE-SO, os mais elevados. Propriedades localizadas mais ao sul do Estado de São Paulo apresentaram menores níveis de doença, provavelmente em consequência da ocorrência recente da doença em tais áreas. em relação à produção, os alinhamentos de plantio N-S e L-O proporcionaram maior número de frutos por planta, assim como quanto ao número de caixas por planta. Por outro lado, a menor produção foi verificada nos alinhamentos NO-SE. em relação à qualidade do suco, não foi possível estabelecer um padrão definido em termos de ratio e ºBrix e os respectivos alinhamentos de plantio. Foi verificado que os valores de ratio foram menores nos frutos de pomares localizados mais ao sul do Estado, de maiores latitudes.