A Be-type star with a black-hole companion

Stellar-mass black holes have all been discovered through X-ray emission, which arises from the accretion of gas from their binary companions (this gas is either stripped from low-mass stars or supplied as winds from massive ones). Binary evolution models also predict the existence of black holes accreting from the equatorial envelope of rapidly spinning Be-type stars (stars of the Be type are hot blue irregular variables showing characteristic spectral emission lines of hydrogen). Of the ~80 Be X-ray binaries known in the Galaxy, however, only pulsating neutron stars have been found as companions. A black hole was formally allowed as a solution for the companion to the Be star MWC 656 (also known as HD 215227), although that was based on a single radial velocity curve of the Be star, a mistaken spectral classification and rough estimates of the inclination angle. Here we report observations of an accretion disk line mirroring the orbit of the Be star. This, together with an improved radial velocity curve of the Be star through fitting sharp Fe II profiles from the equatorial disk, and a refined Be classification (to that of a B1.5-B2 III star), reveals a black hole of 3.8 to 6.9 solar masses orbiting MWC 656, the candidate counterpart of the gamma-ray source AGL J2241+4454. The black hole is X-ray quiescent and fed by a radiatively inefficient accretion flow giving a luminosity less than 1.6 x 10-7 times the Eddington luminosity. This implies that Be binaries with black-hole companions are difficult to detect by conventional X-ray surveys.

An Analysis of Eye Scanpath Entropy in a Progressively Forming Virtual Environment

A sign of presence in virtual environments is that people respond to situations and events as if they were real, where response may be considered at many different levels, ranging from unconscious physiological responses through to overt behavior,emotions, and thoughts. In this paper we consider two responses that gave different indications of the onset of presence in a gradually forming environment. Two aspects of the response of people to an immersive virtual environment were recorded: their eye scanpath, and their skin conductance response (SCR). The scenario was formed over a period of 2 min, by introducing an increasing number of its polygons in random order in a head-tracked head-mounted display. For one group of experimental participants (n 8) the environment formed into one in which they found themselves standing on top of a 3 m high column. For a second group of participants (n 6) the environment was otherwise the same except that the column was only 1 cm high, so that they would be standing at normal ground level. For a third group of participants (n 14) the polygons never formed into a meaningful environment. The participants who stood on top of the tall column exhibited a significant decrease in entropy of the eye scanpath and an increase in the number of SCR by 99 s into the scenario, at a time when only 65% of the polygons had been displayed. The ground level participants exhibited a similar decrease in scanpath entropy, but not the increase in SCR. The random scenario grouping did not exhibit this decrease in eye scanpath entropy. A drop in scanpath entropy indicates that the environment had cohered into a meaningful perception. An increase in the rate of SCR indicates the perception of an aversive stimulus. These results suggest that on these two dimensions (scanpath entropy and rate of SCR) participants were responding realistically to the scenario shown in the virtual environment. In addition, the response occurred well before the entire scenario had been displayed, suggesting that once a set of minimal cues exists within a scenario,it is enough to form a meaningful perception. Moreover, at the level of the sympathetic nervous system, the participants who were standing on top of the column exhibited arousal as if their experience might be real. This is an important practical aspect of the concept of presence.

Produção de mudas de caramboleiras 'B-10' e 'Golden Star': I - parâmetros biológicos

O Brasil é um dos maiores produtores de carambola do mundo, entretanto há poucas informações científicas, especialmente estudos de nutrição mineral com mudas dessa frutífera. Objetivando contribuir com o conhecimento desse importante aspecto, desenvolveu-se estudo que permitisse avaliar o crescimento e o acúmulo de nutrientes em mudas de caramboleiras, cultivadas em solução nutritiva. O experimento foi realizado em parcelas subdivididas, sendo utilizadas como parcela as duas cultivares de caramboleira ('B-10' e 'Golden Star') e, como subparcelas, as cinco épocas de coleta de plantas, realizadas aos 208; 233; 258; 283 e 308 dias após o transplantio para a solução nutritiva. O delineamento foi inteiramente casualizado, com três repetições. As mudas foram cultivadas em vasos (8L) com solução nutritiva (pH=5,5 ± 0,5), com aeração. O experimento iniciou-se em 24-08-2005. Nos diferentes órgãos das mudas (folhas, caule e raízes), avaliaram-se o crescimento e o acúmulo de nutrientes, e os índices nutricionais. Não houve diferenças no crescimento e, em geral, no acúmulo da massa da matéria seca entre as duas cultivares. Houve acúmulo linear da massa da matéria seca das mudas de caramboleira com o tempo de cultivo, sendo maior nas folhas > caule > raízes. O período de maior acúmulo da massa de matéria seca e da taxa de crescimento relativo na planta inteira esteve compreendido entre 208 - 233 e 233 - 258 dias após o transplantio para a 'B-10' e a 'Golden Star', respectivamente.

Produção de mudas de caramboleiras 'B-10' e 'Golden Star': II - marcha de absorção e acúmulo de nutrientes

A participação do Brasil no mercado externo de frutas tem aumentado consideravelmente e com potencial para crescer ainda mais. A constante ascensão dos dados de exportação brasileira é resultado da combinação de avanços tecnológicos do setor produtivo e de acesso a novos mercados consumidores. A caramboleira apresenta-se como uma excelente opção de cultivo de frutas exóticas, com grande potencial para atender ao mercado interno e às exportações. Assim, objetivou-se avaliar a marcha de absorção e de acúmulo de nutrientes em mudas de caramboleiras cultivadas em solução nutritiva. O experimento foi realizado em parcelas subdivididas, sendo utilizadas como parcela as duas cultivares de caramboleira ('B-10' e 'Golden Star') e, como subparcelas, cinco épocas de coleta de plantas, realizadas aos 208; 233; 258; 283 e 308 dias após o transplantio para a solução nutritiva. O delineamento foi inteiramente casualizado, com três repetições. As mudas foram cultivadas em vasos (8L) com solução nutritiva (pH=5,5 ± 0,5), com aeração. O experimento iniciou-se em 24-08-2005. Nos diferentes órgãos das mudas (folhas, caule e raízes), determinaram-se a marcha de absorção, o acúmulo de nutrientes e os índices nutricionais. Não houve diferenças no acúmulo de nutrientes entre as mudas de caramboleira de ambas as cultivares, sendo a ordem decrescente dos nutrientes em cada muda de 'B-10', no final do período experimental: N > K > Ca > Mg > S > P > Fe > Mn > B > Cu > Zn. Para a 'Golden Star', a ordem foi: N > K > Ca > Mg > P > S > Fe > Mn > B > Cu > Zn. Para as duas cultivares, o acúmulo médio foi maior nas folhas > caule > raízes. O período de maior exigência para 'B-10' foi entre 208 - 233 e, para 'Golden Star', entre 233 - 283 dias após o transplantio. As diferentes taxas de acumulação líquida dos nutrientes, nos diferentes órgãos da caramboleira, nem sempre acompanharam a taxa de acumulação de nutrientes do respectivo órgão.

Gaia photometry for white dwarfs

Context. White dwarfs can be used to study the structure and evolution of the Galaxy by analysing their luminosity function and initial mass function. Among them, the very cool white dwarfs provide the information for the early ages of each population. Because white dwarfs are intrinsically faint only the nearby (~ 20 pc) sample is reasonably complete. The Gaia space mission will drastically increase the sample of known white dwarfs through its 5-6 years survey of the whole sky up to magnitude V = 20-25. Aims. We provide a characterisation of Gaia photometry for white dwarfs to better prepare for the analysis of the scientific output of the mission. Transformations between some of the most common photometric systems and Gaia passbands are derived. We also give estimates of the number of white dwarfs of the different galactic populations that will be observed. Methods. Using synthetic spectral energy distributions and the most recent Gaia transmission curves, we computed colours of three different types of white dwarfs (pure hydrogen, pure helium, and mixed composition with H/He = 0.1). With these colours we derived transformations to other common photometric systems (Johnson-Cousins, Sloan Digital Sky Survey, and 2MASS). We also present numbers of white dwarfs predicted to be observed by Gaia. Results. We provide relationships and colour-colour diagrams among different photometric systems to allow the prediction and/or study of the Gaia white dwarf colours. We also include estimates of the number of sources expected in every galactic population and with a maximum parallax error. Gaia will increase the sample of known white dwarfs tenfold to about 200 000. Gaia will be able to observe thousands of very cool white dwarfs for the first time, which will greatly improve our understanding of these stars and early phases of star formation in our Galaxy.

'Black star': uma mutação somática natural da uva fina de mesa cv. Brasil

A uva fina de mesa 'Black Star', originada de uma mutação somática da uva cv. Brasil em Marialva-PR, é descrita quanto às suas principais características físico-químicas e produtivas. Suas bagas, com sementes, apresentam formato elipsoide alongado com coloração vermelho-escura, tendendo ao preto durante a maturação plena. O ciclo, o desempenho produtivo e a suscetibilidade às doenças fúngicas assemelham-se aos da cv. Itália. Durante a maturação plena, apresenta teor médio de sólidos solúveis de 14ºBrix, 0,6% de ácido tartárico e índice de maturação de 21. Trata-se de nova cultivar de uva fina de mesa com potencial de cultivo no Brasil.

Star et personnage dans la genèse filmique: Edwige Feuillère chez Autant-Lara (1954-1958)

A 47 ans, Edwige Feuillère est la vedette principale du Blé en herbe (1954), où elle incarne une femme d'âge mûr qui entreprend l'initiation amoureuse d'un jeune homme ; quatre ans plus tard, elle joue dans En cas de malheur le rôle d'une épouse qui, dans l'abnégation la plus complète, accepte les infidélités de son mari et s'efface devant le couple formé par Jean Gabin (54 ans) et Brigitte Bardot (24 ans). La place accordée aux deux personnages interprétés par Feuillère sera examinée en termes de construction de l'image d'une star vieillissante à travers l'étude du triangle amoureux qui structure le récit de ces deux adaptations (qu'il s'agira de comparer aux romans de Colette et de Simenon dont elles sont issues), de la stratégie promotionnelle pratiquée et des discours émis à propos de Feuillère au sein de la réception critique. Le contexte de production des films ainsi que certaines versions non retenues du scénario seront discutées à partir des archives du fonds Claude Autant-Lara de la Cinémathèque suisse.

The Besançon Galaxy Model renewed. I. Constraints on the Galactic thin disc evolution from Tycho data

Context. The understanding of Galaxy evolution can be facilitated by the use of population synthesis models, which allow to test hypotheses on the star formation history, star evolution, as well as chemical and dynamical evolution of the Galaxy. Aims. The new version of the Besanc¸on Galaxy Model (hereafter BGM) aims to provide a more flexible and powerful tool to investigate the Initial Mass Function (IMF) and Star Formation Rate (SFR) of the Galactic disc. Methods. We present a new strategy for the generation of thin disc stars which assumes the IMF, SFR and evolutionary tracks as free parameters. We have updated most of the ingredients for the star count production and, for the first time, binary stars are generated in a consistent way. We keep in this new scheme the local dynamical self-consistency as in Bienayme et al (1987). We then compare simulations from the new model with Tycho-2 data and the local luminosity function, as a first test to verify and constrain the new ingredients. The effects of changing thirteen different ingredients of the model are systematically studied. Results. For the first time, a full sky comparison is performed between BGM and data. This strategy allows to constrain the IMF slope at high masses which is found to be close to 3.0, excluding a shallower slope such as Salpeter"s one. The SFR is found decreasing whatever IMF is assumed. The model is compatible with a local dark matter density of 0.011 M pc−3 implying that there is no compelling evidence for significant amount of dark matter in the disc. While the model is fitted to Tycho2 data, a magnitude limited sample with V<11, we check that it is still consistent with fainter stars. Conclusions. The new model constitutes a new basis for further comparisons with large scale surveys and is being prepared to become a powerful tool for the analysis of the Gaia mission data.

Initiation of rivaroxaban in patients with nonvalvular atrial fibrillation at the primary care level: the Swiss Therapy in Atrial Fibrillation for the Regulation of Coagulation (STAR) Study.

BACKGROUND: Rivaroxaban has become an alternative to vitamin-K antagonists (VKA) for stroke prevention in non-valvular atrial fibrillation (AF) patients due to its favourable risk-benefit profile in the restrictive setting of a large randomized trial. However in the primary care setting, physician's motivation to begin with rivaroxaban, treatment satisfaction and the clinical event rate after the initiation of rivaroxaban are not known. METHODS: Prospective data collection by 115 primary care physicians in Switzerland on consecutive nonvalvular AF patients with newly established rivaroxaban anticoagulation with 3-month follow-up. RESULTS: We enrolled 537 patients (73±11years, 57% men) with mean CHADS2 and HAS-BLED-scores of 2.2±1.3 and 2.4±1.1, respectively: 301(56%) were switched from VKA to rivaroxaban (STR-group) and 236(44%) were VKA-naïve (VN-group). Absence of routine coagulation monitoring (68%) and fixed-dose once-daily treatment (58%) were the most frequent criteria for physicians to initiate rivaroxaban. In the STR-group, patient's satisfaction increased from 3.6±1.4 under VKA to 5.5±0.8 points (P<0.001), and overall physician satisfaction from 3.9±1.3 to 5.4±0.9 points (P<0.001) at 3months of rivaroxaban therapy (score from 1 to 6 with higher scores indicating greater satisfaction). In the VN-group, both patient's (5.4±0.9) and physician's satisfaction (5.5±0.7) at follow-up were comparable to the STR-group. During follow-up, 1(0.19%; 95%CI, 0.01-1.03%) ischemic stroke, 2(0.37%; 95%CI, 0.05-1.34%) major non-fatal bleeding and 11(2.05%; 95%CI, 1.03-3.64%) minor bleeding complications occurred. Rivaroxaban was stopped in 30(5.6%) patients, with side effects being the most frequent reason. CONCLUSION: Initiation of rivaroxaban for patients with nonvalvular AF by primary care physicians was associated with a low clinical event rate and with high overall patient's and physician's satisfaction.

Optical characterization of sol-gel glasses derived from Eu3+ complex-forming precursors

Fabrication of new optical devices based upon the incorporation of rare earth ions via sol-gel methods depends on elimination of dopant ion clusters and residual hydroxyl groups from the final material. The optical absorption and/or luminescence properties of luminescent rare earth ions are influenced by the local bonding environment and the distribution of the rare-earth dopants in the matrix. Typically, dopants are incorporated into gel via dissolution of soluble species into the initial precursor sol. In this work, Eu3+ is used as optical probe, to assess changes in the local environment. Results of emission, excitation, fluorescence line narrowing and lifetimes studies of Eu3+-doped gels derived from Si(OCH3)4 and fluorinated/chelate Eu3+ precursors are presented. The precursors used in the sol-gel synthesis were: tris (6,6,7,7,8,8,8-heptafluoro-2,2-dimethyl-3,5-octanedionate) Eu(III), Eu (III) trifluoromethanesulfonate, Eu(III) acetylacetonate hydrate, Eu (III) trifluoroacetate trihidrate, tris (2,2,6,6-tetramethyl-3,5- heptanedionate) Eu(III) and Eu(NO3)3.6H2O. The results were interpreted in terms of the evolution of the Eu3+ fluorescence in systems varying from solution to the gels densified to 800ºC. The lifetimes studies indicate that the fluorinated precursors are effective at reducing the water content in densified gels.

Fragmentation of massive dense cores down to <~ 1000 AU: relation between fragmentation and density structure

In order to shed light on the main physical processes controlling fragmentation of massive dense cores, we present a uniform study of the density structure of 19 massive dense cores, selected to be at similar evolutionary stages, for which their relative fragmentation level was assessed in a previous work. We inferred the density structure of the 19 cores through a simultaneous fit of the radial intensity profiles at 450 and 850 μm (or 1.2 mm in two cases) and the spectral energy distribution, assuming spherical symmetry and that the density and temperature of the cores decrease with radius following power-laws. Even though the estimated fragmentation level is strictly speaking a lower limit, its relative value is significant and several trends could be explored with our data. We find a weak (inverse) trend of fragmentation level and density power-law index, with steeper density profiles tending to show lower fragmentation, and vice versa. In addition, we find a trend of fragmentation increasing with density within a given radius, which arises from a combination of flat density profile and high central density and is consistent with Jeans fragmentation. We considered the effects of rotational-to-gravitational energy ratio, non-thermal velocity dispersion, and turbulence mode on the density structure of the cores, and found that compressive turbulence seems to yield higher central densities. Finally, a possible explanation for the origin of cores with concentrated density profiles, which are the cores showing no fragmentation, could be related with a strong magnetic field, consistent with the outcome of radiation magnetohydrodynamic simulations.

The modular forming press for paperboard packages

In this master’s thesis the structural and functional features of a forming tool are developed to meet the needs of modern packaging production for paperboard packaging are studied. The goal of the study is to develop a new type of machine for the manufacture of the paperboard package by pressing. In the structure of the developed forming press the possibility to modify the packaging as well as the requirements of industrial production, food hygiene and other operational matters are accounted for. The press has been sized based on the main dimensions of a single food-grade paperboard tray. In the LUT Packaging Laboratory the forming press is designed suitable for on-line operation. In addition, suggestions for further development of packaging line and equipment have been made based on the information gathered during this thesis study.

Leaving the Dark ages with AMIGA

We present an Analytic Model of Intergalactic-medium and GAlaxy (AMIGA) evolution since the dark ages. AMIGA is in the spirit of the popular semi-analytic models of galaxy formation, although it does not use halo merger trees but interpolates halo properties in grids that are progressively built. This strategy is less memory-demanding and allows one to start modeling at sufficiently high redshifts and low halo masses to have trivial boundary conditions. The number of free parameters is minimized by making a causal connection between physical processes usually treated as independent of each other, which leads to more reliable predictions. However, the strongest points of AMIGA are the following: (1) the inclusion of molecular cooling and metal-poor, population III (Pop III) stars with the most dramatic feedback and (2) accurate follow up of the temperature and volume filling factor of neutral, singly ionized, and doubly ionized regions, taking into account the distinct halo mass functions in those environments. We find the following general results. Massive Pop III stars determine the intergalactic medium metallicity and temperature, and the growth of spheroids and disks is self-regulated by that of massive black holes (MBHs) developed from the remnants of those stars. However, the properties of normal galaxies and active galactic nuclei appear to be quite insensitive to Pop III star properties due to the much higher yield of ordinary stars compared to Pop III stars and the dramatic growth of MBHs when normal galaxies begin to develop, which cause the memory loss of the initial conditions.

Combining genetic and demographic data for the conservation of a Mediterranean habitat-forming species

The integration of ecological and evolutionary data is highly valuable for conservation planning. However, it has been rarely used in the marine realm, where the adequate design of marine protected areas (MPAs) is urgently needed. Here, we examined the interacting processes underlying the patterns of genetic structure and demographic strucuture of a highly vulnerable Mediterranean habitat-forming species (i.e. Paramuricea clavata (Risso, 1826)), with particular emphasis on the processes of contemporary dispersal, genetic drift, and colonization of a new population. Isolation by distance and genetic discontinuities were found, and three genetic clusters were detected; each submitted to variations in the relative impact of drift and gene flow. No founder effect was found in the new population. The interplay of ecology and evolution revealed that drift is strongly impacting the smallest, most isolated populations, where partial mortality of individuals was highest. Moreover, the eco-evolutionary analyses entailed important conservation implications for P. clavata. Our study supports the inclusion of habitat-forming organisms in the design of MPAs and highlights the need to account for genetic drift in the development of MPAs. Moreover, it reinforces the importance of integrating genetic and demographic data in marine conservation.