Strong electrostatic interaction effect on modulational stability of dust acoustic waves

The modulational instability of dust-acoustic waves is investigated, relying on a recently proposed model for strong electrostatic interactions between the highly charged dust particles. The resulting effect on the occurrence (threshold, growth rate) of modulational instability is investigated. Our results can in principle be tested experimentally.

Rat clonidine mydriasis model:Imidazoline receptors are not involved

The clonidine mydriasis model in rats has been widely applied in preclinical research to characterize a -adrenoceptor antagonistic properties of drugs. The present study was undertaken to pharmacologically determine if imidazoline I receptors are also involved in this model system. Sigmoid dose-response curves for pupillary dilation were produced in pentobarbital anesthetized rats by intravenous administration of increasing doses of agonists (guanabenz for a -adrenoceptors, clonidine for both a - adrenoceptors and imidazoline I receptors, and rilmenidine for imidazoline I receptors). Two antagonists (RS 79948 for a -adrenoceptors and efaroxan for imidazoline I receptors) were used to antagonize the mydriasis elicited by those three agonists, with antagonistic potencies calculated. In additional experiments, we examined the effect of the selective imidazoline I receptor antagonist, AGN 192403, on clonidine-induced mydriasis. The results showed that pupillary response curves elicited by guanabenz, clonidine and rilmenidine were competitively antagonized by both RS 79948 (0.03-1 mg/kg) and efaroxan (0.03-1 mg/kg) in a dose-related fashion. The potencies of either antagonist against the three agonists were not significantly different. AGN 192403 (5 mg/kg) did not significantly shift the clonidine mydriasis curve. These results suggest that imidazoline I receptors are not functionally involved in the rat clonidine mydriasis model and support this in vivo system as a useful model for studies of a -adrenoceptors. © 2004 Elsevier B.V. All rights reserved.

A simple disc wind model for broad absorption line quasars

Approximately 20 per cent of quasi-stellar objects (QSOs) exhibit broad, blue-shifted absorption lines in their ultraviolet spectra. Such features provide clear evidence for significant outflows from these systems, most likely in the form of accretion disc winds. These winds may represent the ‘quasar’ mode of feedback that is often invoked in galaxy formation/evolution models, and they are also key to unification scenarios for active galactic nuclei (AGN) and QSOs. To test these ideas, we construct a simple benchmark model of an equatorial, biconical accretion disc wind in a QSO and use a Monte Carlo ionization/radiative transfer code to calculate the ultraviolet spectra as a function of viewing angle. We find that for plausible outflow parameters, sightlines looking directly into the wind cone do produce broad, blue-shifted absorption features in the transitions typically seen in broad absorption line (BAL) QSOs. However, our benchmark model is intrinsically X-ray weak in order to prevent overionization of the outflow, and the wind does not yet produce collisionally excited line emission at the level observed in non-BAL QSOs. As a first step towards addressing these shortcomings, we discuss the sensitivity of our results to changes in the assumed X-ray luminosity and mass-loss rate, Ṁwind. In the context of our adopted geometry, Ṁwind ∼ Ṁacc is required in order to produce significant BAL features. The kinetic luminosity and momentum carried by such outflows would be sufficient to provide significant feedback.

Line-driven Disk Winds in Activ Galactic Nuclei: The Critical Importance of Ionization and Radiative Transfer

Accretion disk winds are thought to produce many of the characteristic features seen in the spectra of active galactic nuclei (AGNs) and quasi-stellar objects (QSOs). These outflows also represent a natural form of feedback between the central supermassive black hole and its host galaxy. The mechanism for driving this mass loss remains unknown, although radiation pressure mediated by spectral lines is a leading candidate. Here, we calculate the ionization state of, and emergent spectra for, the hydrodynamic simulation of a line-driven disk wind previously presented by Proga & Kallman. To achieve this, we carry out a comprehensive Monte Carlo simulation of the radiative transfer through, and energy exchange within, the predicted outflow. We find that the wind is much more ionized than originally estimated. This is in part because it is much more difficult to shield any wind regions effectively when the outflow itself is allowed to reprocess and redirect ionizing photons. As a result, the calculated spectrum that would be observed from this particular outflow solution would not contain the ultraviolet spectral lines that are observed in many AGN/QSOs. Furthermore, the wind is so highly ionized that line driving would not actually be efficient. This does not necessarily mean that line-driven winds are not viable. However, our work does illustrate that in order to arrive at a self-consistent model of line-driven disk winds in AGN/QSO, it will be critical to include a more detailed treatment of radiative transfer and ionization in the next generation of hydrodynamic simulations.

Herschel key program HERITAGE:A far-infrared source catalog for the Magellanic Clouds

Observations from the HERschel Inventory of the Agents of Galaxy Evolution (HERITAGE ) have been used to identify dusty populations of sources in the Large and Small Magellanic Clouds (LMC and SMC). We conducted the study using the HERITAGE catalogs of point sources available from the Herschel Science Center from both the Photodetector Array Camera and Spectrometer (PACS; 100 and 160 μm) and Spectral and Photometric Imaging Receiver (SPIRE; 250, 350, and 500 μm) cameras. These catalogs are matched to each other to create a Herschel band-merged catalog and then further matched to archival Spitzer IRAC and MIPS catalogs from the Spitzer Surveying the Agents of Galaxy Evolution (SAGE) and SAGE-SMC surveys to create single mid- to far-infrared (far-IR) point source catalogs that span the wavelength range from 3.6 to 500 μm. There are 35,322 unique sources in the LMC and 7503 in the SMC. To be bright in the FIR, a source must be very dusty, and so the sources in the HERITAGE catalogs represent the dustiest populations of sources. The brightest HERITAGE sources are dominated by young stellar objects (YSOs), and the dimmest by background galaxies. We identify the sources most likely to be background galaxies by first considering their morphology (distant galaxies are point-like at the resolution of Herschel) and then comparing the flux distribution to that of the Herschel Astrophysical Terahertz Large Area Survey (ATLAS ) survey of galaxies. We find a total of 9745 background galaxy candidates in the LMC HERITAGE images and 5111 in the SMC images, in agreement with the number predicted by extrapolating from the ATLAS flux distribution. The majority of the Magellanic Cloud-residing sources are either very young, embedded forming stars or dusty clumps of the interstellar medium. Using the presence of 24 μm emission as a tracer of star formation, we identify 3518 YSO candidates in the LMC and 663 in the SMC. There are far fewer far-IR bright YSOs in the SMC than the LMC due to both the SMC's smaller size and its lower dust content. The YSO candidate lists may be contaminated at low flux levels by background galaxies, and so we differentiate between sources with a high ("probable") and moderate ("possible ") likelihood of being a YSO. There are 2493/425 probable YSO candidates in the LMC/SMC. Approximately 73% of the Herschel YSO candidates are newly identified in the LMC, and 35% in the SMC. We further identify a small population of dusty objects in the late stages of stellar evolution including extreme and post-asymptotic giant branch, planetary nebulae, and supernova remnants. These populations are identified by matching the HERITAGE catalogs to lists of previously identified objects in the literature. Approximately half of the LMC sources and one quarter of the SMC sources are too faint to obtain accurate ample FIR photometry and are unclassified.

Spitzer infrared spectrograph point source classification in the Small Magellanic Cloud

The Magellanic Clouds are uniquely placed to study the stellar contribution to dust emission. Individual stars can be resolved in these systems even in the mid-infrared, and they are close enough to allow detection of infrared excess caused by dust. We have searched the Spitzer Space Telescope data archive for all Infrared Spectrograph (IRS) staring-mode observations of the Small Magellanic Cloud (SMC) and found that 209 Infrared Array Camera (IRAC) point sources within the footprint of the Surveying the Agents of Galaxy Evolution in the Small Magellanic Cloud (SAGE-SMC) Spitzer Legacy programme were targeted, within a total of 311 staring-mode observations. We classify these point sources using a decision tree method of object classification, based on infrared spectral features, continuum and spectral energy distribution shape, bolometric luminosity, cluster membership and variability information. We find 58 asymptotic giant branch (AGB) stars, 51 young stellar objects, 4 post-AGB objects, 22 red supergiants, 27 stars (of which 23 are dusty OB stars), 24 planetary nebulae (PNe), 10 Wolf-Rayet stars, 3 H II regions, 3 R Coronae Borealis stars, 1 Blue Supergiant and 6 other objects, including 2 foreground AGB stars. We use these classifications to evaluate the success of photometric classification methods reported in the literature.

Reframing the Favela, Remapping the City: Territorial Embeddedness and (Trans)locality in “Framing Content” on Brazilian Favela Blogs

In recent years, the internet has become a key site for the portrayal of Rio de Janeiro’s favelas. This article examines blogging by favela residents and argues that digital culture constitutes a vital, and as yet not systematically explored, arena of research on the representation of Rio de Janeiro and its favelas. Based on ethnographically inspired research carried out in 2009–2010, this article examines two examples of blog ‘framing content’ (a sidebar and a static page) encountered during fieldwork, which functioned to establish a concrete link between the posts on the blogs in question, their authors, and a named favela, even when the posts were not explicitly about that favela. At the same time, the framing content also made visible, and affirmed, the translocal connections between that favela, other favelas, and the city as a whole. These illustrative examples from a wider study show how favela bloggers are engaged in resignifying and remapping the relationships between different empirical scales of locality (and associated identities) in Rio de Janeiro, demonstrating the contribution an interdisciplinary approach to the digital texts and practices of favela residents can make to an understanding of the contemporary city and its representational conundrums, from the perspective of ‘ordinary practitioners’.

Localized structures in complex plasmas in the presence of a magnetic field

In this work, the general framework in which fits our investigation is that of modeling the dynamics of dust grains therein dusty plasma (complex plasma) in the presence of electromagnetic fields. The generalized discrete complex Ginzburg-Landau equation (DCGLE) is thus obtained to model discrete dynamical structure in dusty plasma with Epstein friction. In the collisionless limit, the equation reduces to the modified discrete nonlinear Schrödinger equation (MDNLSE). The modulational instability phenomenon is studied and we present the criterion of instability in both cases and it is shown that high values of damping extend the instability region. Equations thus obtained highlight the presence of soliton-like excitation in dusty plasma. We studied the generation of soliton in a dusty plasma taking in account the effects of interaction between dust grains and theirs neighbours. Numerical simulations are carried out to show the validity of analytical approach.

Distribuição por tamanhos do aerosol atmosférico na Península Ibérica

Um dos principais fatores que afetam negativamente a qualidade do ambiente em muitas cidades em todo o mundo é o material particulado (PM). A sua presença na atmosfera pode ter impactos negativos na saúde humana, clima, património edificado e ecossistemas. Muitos dos estudos realizados em áreas urbanas focam apenas as frações respiráveis (PM10 e PM2,5). No entanto, os processos de formação, a identificação das fontes emissoras e os efeitos dependem muito da distribuição granulométrica das partículas. A atenção tem recaído na análise de hidrocarbonetos poliaromáticos (PAHs), devida à sua carcinogenicidade e a informação disponível sobre outros compostos é escassa. O presente estudo consistiu na obtenção do PM distribuído por diferentes frações de tamanho e na análise detalhada da sua composição química, em dois locais urbanos da Península Ibérica (Madrid e Lisboa). Dado que os veículos representam uma das principais fontes emissoras em ambientes urbanos, efetuou-se uma caracterização mais detalhada deste tipo de emissões, conduzindo uma campanha de amostragem num túnel rodoviário (Marquês de Pombal, Lisboa). As amostragens, em ambas as cidades, decorreram durante um mês, quer no verão quer no inverno, em dois locais urbanos distintos, um junto a uma via com influência de tráfego e outro numa área urbana de fundo. No túnel a amostragem foi realizada apenas durante uma semana. Em Madrid e no túnel, o PM foi recolhido utilizando um amostrador de elevado volume com impactor em cascata com quatro tamanhos: 10-2,5, 2,5-0,95, 0,95-0,49 e < 0,49 μm. Em Lisboa, foi utilizado um impactor em cascata com apenas dois tamanhos, 10- 2,5 e < 2,5 μm. As amostras foram quimicamente analisadas e determinadas as concentrações de compostos carbonados (OC, EC e carbonatos), iões inorgânicos solúveis em água (Cl−, NO3−, SO42−, Na+, NH4+, K+, Mg2+, Ca2+),metais e compostos orgânicos. Em Madrid, as concentrações médias de PM10 foram 44 e 48% maiores nas amostras recolhidas junto à estrada do que as de fundo urbano no verão e inverno, respetivamente. A fração grosseira e o PM0,5 apresentaram concentrações mais elevadas no verão do que no inverno devido às condições climatéricas pouco usuais. No verão, as amostragens decorreram num mês em que as temperaturas foram muito elevadas e em que ocorreram vários episódios de intrusão de poeira africana. Durante o período de amostragem de inverno, as temperaturas foram muito baixas e registaram-se vários dias de precipitação quer sob a forma de chuva, quer sob a forma de neve. As situações meteorológicas sinóticas mais comuns, incluindo aquelas que causam o transporte de massas de ar com poeiras Africanas, foram identificadas em ambas as estações do ano. As concentrações mássicas de PM10, EC e OC foram encontrados predominantemente na fração de tamanho ultrafino em ambos os locais de amostragem e estações do ano. Nas restantes frações não se observou nenhuma tendência sazonal. O carbono orgânico secundário (SOC) mostrou um claro padrão sazonal, com concentrações muito mais elevadas no verão do que no inverno, em ambos os lugares. A partir do balanço mássico de iões, observou-se que, no verão, a formação de compostos inorgânicos secundários (SIC) conduziu a um enriquecimento pouco comum de Ca2+ na fração submicrométrica, quer nas amostras de tráfego, quer em fundo urbano. Os alcanos, PAHs, os álcoois e os ácidos foram as classes de compostos orgânicos identificados e quantificados no material particulado. Globalmente, representaram 0,26 e 0,11 μg m−3 no verão e inverno, respetivamente, no local de tráfego e 0,28 e 0,035 μg m−3 na área urbana de fundo. Os diferentes compostos orgânicos também apresentaram padrões sazonais, sugerindo fontes de emissão (e.g. escapes dos veículos e fontes biogénicas) ou processos de formação com contribuições variáveis ao longo do ano. As concentrações de benzoapireno equivalente foram menores que 1 ng m-3 e o risco carcinogénico estimado é baixo. No verão, os maiores enriquecimentos de metais ocorreram na fração submicrométrica, e no inverno na fração grosseira. No verão, os enriquecimentos foram ≥ 80% para o Mn, Ni, Cu, Zn, Cd, Sb e Co, no inverno, estes traçadores de emissões do tráfego foram menores, exceto para o Zn. Em Lisboa, a concentração média de PM10 foi de 48 μg m-3 no verão e de 44 μg m-3 no inverno, junto à estrada. Na área de fundo urbano, registaram-se níveis comparáveis nas duas estações (27 μg m-3 e 26 μg m-3). A média do rácio PM2,5/PM10 foi de 65% no verão e 44% no inverno na área de tráfego e 62% e 59% na área urbana de fundo. Estes resultados significam que o PM2,5 é um dos principais contaminantes que afetam a qualidade do ar no centro da cidade de Lisboa. A relação OC/EC, que reflete a composição das emissões de combustão dos veículos, variou entre 0,3 e 0,4 no interior do túnel. Os rácios de OC/EC mínimos obtidos junto às vias de tráfego em Madrid e em Lisboa encontram-se entre os do túnel e os registados em atmosferas urbanas de fundo, sugerindo que os valores mínimos habitualmente obtidos para este parâmetro em ambientes urbanos abertos sobrestimam as emissões diretas de OC pelo transporte rodoviário. Espera-se que os resultados deste trabalho contribuam para suprir, pelo menos em parte, as lacunas de informação quer sobre a composição de várias granulometrias de PM, quer sobre fontes e processos de formação em atmosferas urbanas. Como a exposição a poluentes do ar ultrapassa o controle dos indivíduos e exige ação das autoridades públicas a nível nacional, regional e até mesmo internacional, é importante propor medidas mitigadoras focadas nas principais fontes de emissão identificadas.

1969-70 Hockey Team

1969-71 Brock Generals Hockey team. Members from left to right - Back row: Tom Kearney (Trainer), Al Kellogg (Coach), John Hull, Craig Morrison, Gregg Law, Frank Mucci, Dale Andreas, Eric Stevens, Serge Girrard, John Clarey, Wayne Kenyon, Reg Egilsson, Dusty Papke, Randy Oiling (Manager). Front row: Ron Powel, Barry Hopkins, Bruce Wormald, Miller Hicks, Fred Carter, Mike Nicholson, Dick Overholt, Chris Shott. Missing: John O'Brien, Barry Elliot.

The effect of pH and ethanol on the astringent sub-qualities of red wine, and the implications for optimum grape maturity /

The first objective of this study was to identify appropriate sensory descriptors to assess the astringent sub-qualities of red wine. The influence of pH and ethanol on the sensation of astringency in red wine was evaluated, using a de-alcoholized red wine. A portion of the wine was adjusted to the pH values of 3.2, 3.4, 3.6 and 3.8, and another portion was adjusted to ethanol concentrations of 0%, 6%, 12%, and 15%. In addition, the pH 3.4 and 3.6 treatments were adjusted to an ethanol concentration of 12% and 15% all wines were then assessed sensorially and seventeen terms were identified, through panel discussion, to describe the mouth-feel and taste qualities: velvet, aggressive, silk/satin, dry, fleshy, unripe, pucker viscosity, abrasive, heat, chewy, acidity, grippy/adhesive, bitter, balance, overall astringency, and mouth-coat. Descriptive analysis profiling techniques were used to train the panel and measure the intensity of these attributes. It was found that decreasing pH values (averaged across all ethanol concentrations) showed an increase in the overall astringency of the wine. The combined treatments of ethanol and pH, real wine parameters (pH 3.4 and 3.6; 12% and 15% ethanol) did not have an effect on the perception of the astringent sub-qualities of the wine. A time intensity study was also included using the pH and ethanol adjusted wines, which showed that as the ethanol level of the wines increased so did the time to maximum intensity. The second objective was to identify appropriate sensory descriptors to evaluate the influence of grape maturity and maceration technique (grape skin contact) on the astringency sub-qualities of red vinifera wines from Niagara. The grapes were harvested across two dates, representing an early harvest and a late harvest. A portion of the Cabernet Sauvignon grapes wine was divided into three maceration treatments of oneweek maceration, standard two-week maceration, three-week maceration, and MCM. Another portion of both the early and late harvest Cabernet Sauvignon grapes were chaptalized to yield a final ethanol concentration of 14.5%. The wines were assessed sensorially and thirteen terms were identified, through panel discussion, to describe the mouth-feel and taste qualities: carbon dioxide, pucker, acidity, silk/chamois, dusty/chalky/powdery, sandpaper, numbing, grippy/adhesive, dry, mouthcoat, bitter, balance and, overall astringency. Descriptive analysis techniques were used to train the panel and measure the intensity of these attributes. The data revealed few significant differences in the mouth-feel of the wines with respect to maturity; which included differences in overall astringency and balance. There were varietal differences between Cabernet Sauvignon, Cabernet Franc, and Pinot Noir and differences for Cabernet Sauvignon wines due to the length and manner of maceration and as a result of chaptalization. Statistical analysis revealed a more complex mouth-feel for the Pinot Noir wines; and an increase in the intensity of the astringent sub-qualities as a result of the addition of sugar to the wines. These findings have implications for how processing decisions, such as optimum grape maturity and vinification methods may affect red wine quality.