Massive open online courses (mooc) na formação contínua de professores: um estudo de caso

Os Massive Open Online Courses (MOOC) consistem em cursos online abertos e, normalmente gratuitos, que permitem a inscrição de um elevado número de participantes. A adesão a esta modalidade de educação, normalmente informal, foi o principal repto para propor uma oficina de formação, totalmente online. Com esta formação pretendeu-se fornecer as competências necessárias para que professores se sentissem capacitados para criar e distribuir os seus próprios MOOC. No presente trabalho recorre-se à metodologia de estudo de caso e procura-se inicialmente apresentar, através de pesquisa bibliográfica, a revisão de literatura relativamente aos MOOC. Posteriormente, com base nos dados obtidos pela observação participante e inquérito por questionário, evidenciam-se os principais resultados da oficina de formação online “MOOC: uma tecnologia educativa de futuro.

A Case of Mesenteric Pseudocyst Causing a Massive Abdominal Swelling

We present the case of a 55-year-old man, with a self-limited febrile condition associated to polyserositis with inconclusive investigation. Bilateral pleural and pericardial effusions resolved. The peritoneal fluid loculated and was compatible with an exudate. The patient remained clinically asymptomatic. Two years later, examination revealed a palpable and painless abdominal mass, which imaging study suggested a cystic lesion. Surgical resection was performed and the histological examination revealed a mesenteric pseudocyst. Mesenteric pseudocysts are rare intra-abdominal cystic masses, mostly benign, without causing specific symptoms. Although imaging tests are useful for their differential diagnosis, the histology is mandatory.

Satisfying the Einstein-Podolsky-Rosen criterion with massive particles

In 1935, Einstein, Podolsky and Rosen (EPR) questioned the completeness of quantum mechanics by devising a quantum state of two massive particles with maximally correlated space and momentum coordinates. The EPR criterion qualifies such continuous-variable entangled states, where a measurement of one subsystem seemingly allows for a prediction of the second subsystem beyond the Heisenberg uncertainty relation. Up to now, continuous-variable EPR correlations have only been created with photons, while the demonstration of such strongly correlated states with massive particles is still outstanding. Here we report on the creation of an EPR-correlated two-mode squeezed state in an ultracold atomic ensemble. The state shows an EPR entanglement parameter of 0.18(3), which is 2.4 s.d. below the threshold 1/4 of the EPR criterion. We also present a full tomographic reconstruction of the underlying many-particle quantum state. The state presents a resource for tests of quantum nonlocality and a wide variety of applications in the field of continuous-variable quantum information and metrology.

An extreme planetary system around HD 219828: one long-period super Jupiter to a hot-Neptune host star

Context. With about 2000 extrasolar planets confirmed, the results show that planetary systems have a whole range of unexpected properties. This wide diversity provides fundamental clues to the processes of planet formation and evolution. Aims: We present a full investigation of the HD 219828 system, a bright metal-rich star for which a hot Neptune has previously been detected. Methods: We used a set of HARPS, SOPHIE, and ELODIE radial velocities to search for the existence of orbiting companions to HD 219828. The spectra were used to characterise the star and its chemical abundances, as well as to check for spurious, activity induced signals. A dynamical analysis is also performed to study the stability of the system and to constrain the orbital parameters and planet masses. Results: We announce the discovery of a long period (P = 13.1 yr) massive (m sini = 15.1 MJup) companion (HD 219828 c) in a very eccentric orbit (e = 0.81). The same data confirms the existence of a hot Neptune, HD 219828 b, with a minimum mass of 21 M⊕ and a period of 3.83 days. The dynamical analysis shows that the system is stable, and that the equilibrium eccentricity of planet b is close to zero. Conclusions: The HD 219828 system is extreme and unique in several aspects. First, ammong all known exoplanet systems it presents an unusually high mass ratio. We also show that systems like HD 219828, with a hot Neptune and a long-period massive companion are more frequent than similar systems with a hot Jupiter instead. This suggests that the formation of hot Neptunes follows a different path than the formation of their hot jovian counterparts. The high mass, long period, and eccentricity of HD 219828 c also make it a good target for Gaia astrometry as well as a potential target for atmospheric characterisation, using direct imaging or high-resolution spectroscopy. Astrometric observations will allow us to derive its real mass and orbital configuration. If a transit of HD 219828 b is detected, we will be able to fully characterise the system, including the relative orbital inclinations. With a clearly known mass, HD 219828 c may become a benchmark object for the range in between giant planets and brown dwarfs.

Time-Reversal Massive Multipath Effect and Bandwidth Heterogeneity

The proliferation of new mobile communication devices, such as smartphones and tablets, has led to an exponential growth in network traffic. The demand for supporting the fast-growing consumer data rates urges the wireless service providers and researchers to seek a new efficient radio access technology, which is the so-called 5G technology, beyond what current 4G LTE can provide. On the other hand, ubiquitous RFID tags, sensors, actuators, mobile phones and etc. cut across many areas of modern-day living, which offers the ability to measure, infer and understand the environmental indicators. The proliferation of these devices creates the term of the Internet of Things (IoT). For the researchers and engineers in the field of wireless communication, the exploration of new effective techniques to support 5G communication and the IoT becomes an urgent task, which not only leads to fruitful research but also enhance the quality of our everyday life. Massive MIMO, which has shown the great potential in improving the achievable rate with a very large number of antennas, has become a popular candidate. However, the requirement of deploying a large number of antennas at the base station may not be feasible in indoor scenarios. Does there exist a good alternative that can achieve similar system performance to massive MIMO for indoor environment? In this dissertation, we address this question by proposing the time-reversal technique as a counterpart of massive MIMO in indoor scenario with the massive multipath effect. It is well known that radio signals will experience many multipaths due to the reflection from various scatters, especially in indoor environments. The traditional TR waveform is able to create a focusing effect at the intended receiver with very low transmitter complexity in a severe multipath channel. TR's focusing effect is in essence a spatial-temporal resonance effect that brings all the multipaths to arrive at a particular location at a specific moment. We show that by using time-reversal signal processing, with a sufficiently large bandwidth, one can harvest the massive multipaths naturally existing in a rich-scattering environment to form a large number of virtual antennas and achieve the desired massive multipath effect with a single antenna. Further, we explore the optimal bandwidth for TR system to achieve maximal spectral efficiency. Through evaluating the spectral efficiency, the optimal bandwidth for TR system is found determined by the system parameters, e.g., the number of users and backoff factor, instead of the waveform types. Moreover, we investigate the tradeoff between complexity and performance through establishing a generalized relationship between the system performance and waveform quantization in a practical communication system. It is shown that a 4-bit quantized waveforms can be used to achieve the similar bit-error-rate compared to the TR system with perfect precision waveforms. Besides 5G technology, Internet of Things (IoT) is another terminology that recently attracts more and more attention from both academia and industry. In the second part of this dissertation, the heterogeneity issue within the IoT is explored. One of the significant heterogeneity considering the massive amount of devices in the IoT is the device heterogeneity, i.e., the heterogeneous bandwidths and associated radio-frequency (RF) components. The traditional middleware techniques result in the fragmentation of the whole network, hampering the objects interoperability and slowing down the development of a unified reference model for the IoT. We propose a novel TR-based heterogeneous system, which can address the bandwidth heterogeneity and maintain the benefit of TR at the same time. The increase of complexity in the proposed system lies in the digital processing at the access point (AP), instead of at the devices' ends, which can be easily handled with more powerful digital signal processor (DSP). Meanwhile, the complexity of the terminal devices stays low and therefore satisfies the low-complexity and scalability requirement of the IoT. Since there is no middleware in the proposed scheme and the additional physical layer complexity concentrates on the AP side, the proposed heterogeneous TR system better satisfies the low-complexity and energy-efficiency requirement for the terminal devices (TDs) compared with the middleware approach.

On neutron stars in ƒ (R) theories: Small radii, large masses and large energy emitted in a merger

In the context of ƒ (R) gravity theories, we show that the apparent mass of a neutron star as seen from an observer at infinity is numerically calculable but requires careful matching, first at the star’s edge, between interior and exterior solutions, none of them being totally Schwarzschild-like but presenting instead small oscillations of the curvature scalar R; and second at large radii, where the Newtonian potential is used to identify the mass of the neutron star. We find that for the same equation of state, this mass definition is always larger than its general relativistic counterpart. We exemplify this with quadratic R^2 and Hu-Sawicki-like modifications of the standard General Relativity action. Therefore, the finding of two-solar mass neutron stars basically imposes no constraint on stable ƒ (R) theories. However, star radii are in general smaller than in General Relativity, which can give an observational handle on such classes of models at the astrophysical level. Both larger masses and smaller matter radii are due to much of the apparent effective energy residing in the outer metric for scalar-tensor theories. Finally, because the ƒ (R) neutron star masses can be much larger than General Relativity counterparts, the total energy available for radiating gravitational waves could be of order several solar masses, and thus a merger of these stars constitutes an interesting wave source.

Topological massive Dirac edge modes and long-range superconducting Hamiltonians

We discover novel topological effects in the one-dimensional Kitaev chain modified by long-range Hamiltonian deformations in the hopping and pairing terms. This class of models display symmetry-protected topological order measured by the Berry/Zak phase of the lower-band eigenvector and the winding number of the Hamiltonians. For exponentially decaying hopping amplitudes, the topological sector can be significantly augmented as the penetration length increases, something experimentally achievable. For power-law decaying superconducting pairings, the massless Majorana modes at the edges get paired together into a massive nonlocal Dirac fermion localized at both edges of the chain: a new topological quasiparticle that we call topological massive Dirac fermion. This topological phase has fractional topological numbers as a consequence of the long-range couplings. Possible applications to current experimental setups and topological quantum computation are also discussed.

Ratio of hemocomponents in massive transfusion and mortality of trauma patients in a university hospital

Background: Nowadays, there are very few studies about massive transfusion in our country. This situation generates the necessity to the elevation of possible new strategies to diminish mortality and its adverse effects. Material and methods: All massive transfusions were evaluated in a retrospective way from October 2010 to October 2012. All diagnosis groups were recorded and the patients were divided into three groups depending on the ratio between packed red blood cells (PRBC) and fresh frozen plasma (FFP) units (ratios ≤2, >2, and without FFP). Their mortality and/or survival were evaluated 30 days after as well as all the factors associated with the event. Results: A total of 69 patients were included (37 trauma patients, 28 gunshot wounds and 4 with lacerated wounds); the groups (ratios ≤2, >2, and no plasma at all) were distributed as follows: 30, 30 and 9 patients each, with an overall mortality rate of 60.8% within 30 days. A lower survival rate (12%) in the no plasma group (P=.015) was found and systolic blood pressure during transfusion had a mean of 67.7 mmHg (P=.012) in this group. Fresh frozen plasma units were 136 and 249 for >2 and ≤2 ratios respectively (P<.01); 85.5% of all patients developed metabolic acidosis during the transfusion, and the number of days in the hospital after the event had a mean of 24.5 days in all patients. Conclusions: High rates of massive transfusion mortality are still being reported in our ield. The use of transfusion strategies contribute to elevate the survival rate in patients with massive transfusion treatment

Early Adaptation of Small Intestine After Massive Small Bowel Resection in Rats

Background: It is important that the residual bowel adapts after massive resection. The necessary intestinal adaptation is a progressive recovery from intestinal failure through increase in absorptive surface area and functional capacity and includes both morphological and functional adaptations. Objectives: The aim of this study was to investigate intestinal morphological and functional adaptations of small bowel syndrome (SBS) model rats (SBS1W) 7 days after bowel resection. Materials and Methods: Male sprague–dawley rats (n = 20/group) underwent either a 75% proximal small bowel resection (SBS1W group) or a control operation (control group). Markers of morphological adaptation were revealed by TEM analysis of H&E-stained tissue samples. The intestinal barrier condition was assessed by BT, and sIgA concentration in intestinal mucus was measured by ELISA. Contractility and the slow wave rhythm of the entire intestinal remnant were measured and recorded. Results: The SBS1W group experienced more weight loss than control group and had a clearly different intestinal morphology as revealed in TEM images. Compared with control rats, the SBS1W group had a lower sIgA concentration in intestinal mucus and higher BT to lymph nodes (70% vs 40%; level I), portal blood (40% vs 10%; level II), and peripheral blood (60% vs 30%; level III). Disorder of spontaneous rhythmic contraction, irregular amplitude, and slow frequency were detected in the SBS1W group by a muscle strips test. Similarly, the slow wave of the entire intestinal remnant in the SBS1W group was irregular and uncoordinated. Conclusions: The finding of intestinal adaptation following massive SBR in SBS1W rats provides more understanding of the mechanisms of progressive recovery from the intestinal failure that underlies SBS. The mechanical, chemical, immunological, and biological barriers were all impaired at 7 days following bowel resection, indicating that the SBS model rats were still in the intestinal adaptation phase.

Recherche et analyse d'étoiles naines blanches chimiquement stratiées dans le Sloan Digital Sky Survey

Ce mémoire présente une recherche détaillée et une analyse des étoiles naines blanches hybrides chimiquement stratifiées dans le Sloan Digital Sky Survey (SDSS). Une seule étoile stratifiée, PG 1305-017, était connue avant notre recherche. L'objectif principal est de confirmer l'existence de plusieurs nouvelles étoiles stratifiées. Pour ce faire, il a fallu dans un premier temps développer une nouvelle génération de modèles d'atmosphère à partir de ceux de Bergeron et al. (1991) et Tremblay & Bergeron (2009). Nous y avons ajouté l'opacité de toutes les raies d'hélium et les calculs nécessaires pour tenir compte de la stratification chimique de l'atmosphère, où une mince quantité d’hydrogène flotte en équilibre diffusif au-dessus d’une enveloppe massive d’hélium. En parallèle, nous avons aussi calculé des modèles standards, chimiquement homogènes. Ensuite, nous avons sélectionné des naines blanches chaudes (Teff > 30,000 K) de type spectral hybride (traces d'hélium et d'hydrogène) parmi les ~38,000 naines blanches répertoriées dans le SDSS. Un total de 52 spectres d'étoile a été retenu dans notre échantillon final. La technique spectroscopique, c'est-à-dire l'ajustement des raies spectrales des modèles sur un spectre observé, a été appliquée à toutes les étoiles de notre échantillon. Nous avons ainsi mesuré la température effective, la gravité de surface et la composition chimique de l'atmosphère de ces étoiles. Par l'ajustement simultané de modèles stratifiés et homogènes, nous avons aussi pu déterminer si les étoiles étaient stratifiées ou non. Nous identifions ainsi 14 naines blanches stratifiées. Nous tirons de ces résultats plusieurs conclusions sur les processus physiques expliquant la présence d'hélium dans l'atmosphère.

Recherche et analyse d'étoiles naines blanches chimiquement stratiées dans le Sloan Digital Sky Survey

Ce mémoire présente une recherche détaillée et une analyse des étoiles naines blanches hybrides chimiquement stratifiées dans le Sloan Digital Sky Survey (SDSS). Une seule étoile stratifiée, PG 1305-017, était connue avant notre recherche. L'objectif principal est de confirmer l'existence de plusieurs nouvelles étoiles stratifiées. Pour ce faire, il a fallu dans un premier temps développer une nouvelle génération de modèles d'atmosphère à partir de ceux de Bergeron et al. (1991) et Tremblay & Bergeron (2009). Nous y avons ajouté l'opacité de toutes les raies d'hélium et les calculs nécessaires pour tenir compte de la stratification chimique de l'atmosphère, où une mince quantité d’hydrogène flotte en équilibre diffusif au-dessus d’une enveloppe massive d’hélium. En parallèle, nous avons aussi calculé des modèles standards, chimiquement homogènes. Ensuite, nous avons sélectionné des naines blanches chaudes (Teff > 30,000 K) de type spectral hybride (traces d'hélium et d'hydrogène) parmi les ~38,000 naines blanches répertoriées dans le SDSS. Un total de 52 spectres d'étoile a été retenu dans notre échantillon final. La technique spectroscopique, c'est-à-dire l'ajustement des raies spectrales des modèles sur un spectre observé, a été appliquée à toutes les étoiles de notre échantillon. Nous avons ainsi mesuré la température effective, la gravité de surface et la composition chimique de l'atmosphère de ces étoiles. Par l'ajustement simultané de modèles stratifiés et homogènes, nous avons aussi pu déterminer si les étoiles étaient stratifiées ou non. Nous identifions ainsi 14 naines blanches stratifiées. Nous tirons de ces résultats plusieurs conclusions sur les processus physiques expliquant la présence d'hélium dans l'atmosphère.

Realización y difusión de un Massive Open Online Course de narrativa audiovisual avanzada: el alumnado como creador de recursos educativos abiertos

El objetivo fundamental es continuar con la creación de un Massive Open OnlineCourse (MOOC) de narrativa audiovisual diseñado por profesorado y alumnado elaborando materiales videográficos e hipermedia innovadores para su difusión abierta.

Incidence of debris discs around FGK stars in the solar neighbourhood

Context. Debris discs are a consequence of the planet formation process and constitute the fingerprints of planetesimal systems. Their counterparts in the solar system are the asteroid and Edgeworth-Kuiper belts. Aims. The aim of this paper is to provide robust numbers for the incidence of debris discs around FGK stars in the solar neighbourhood. Methods. The full sample of 177 FGK stars with d ≤ 20 pc proposed for the DUst around NEarby Stars (DUNES) survey is presented. Herschel/PACS observations at 100 and 160 μm were obtained, and were complemented in some cases with data at 70 μm and at 250, 350, and 500 μm SPIRE photometry. The 123 objects observed by the DUNES collaboration were presented in a previous paper. The remaining 54 stars, shared with the Disc Emission via a Bias-free Reconnaissance in IR and Sub-mm (DEBRIS) consortium and observed by them, and the combined full sample are studied in this paper. The incidence of debris discs per spectral type is analysed and put into context together with other parameters of the sample, like metallicity, rotation and activity, and age. Results. The subsample of 105 stars with d ≤ 15 pc containing 23 F, 33 G, and 49 K stars is complete for F stars, almost complete for G stars, and contains a substantial number of K stars from which we draw solid conclusions on objects of this spectral type. The incidence rates of debris discs per spectral type are 0.26^+0.21_-0.14 (6 objects with excesses out of 23 F stars), 0.21^+0.17_-0.11 (7 out of 33 G stars), and 0.20^+0.14_-0.09 (10 out of 49 K stars); the fraction for all three spectral types together is 0.22^+0.08_-0.07 (23 out of 105 stars). The uncertainties correspond to a 95% confidence level. The medians of the upper limits of L_dust/L_∗ for each spectral type are 7.8 × 10^-7 (F), 1.4 × 10^-6 (G), and 2.2 × 10^-6 (K); the lowest values are around 4.0 × 10^-7. The incidence of debris discs is similar for active (young) and inactive (old) stars. The fractional luminosity tends to drop with increasing age, as expected from collisional erosion of the debris belts.

Unveiling the unknown of cool stars with high-resolution spectroscopy

Cool giant and supergiant stars are among the brightest populations in any stellar system and they are easily observable out to large distances, especially at infrared wavelengths. These stars also dominate the integrated light of star clusters in a wide range of ages, making them powerful tracers of stellar populations in more distant galaxies. High-resolution near-IR spectroscopy is a key tool for quantitatively investigating their kinematic, evolutionary and chemical properties. However, the systematic exploration and calibration of the NIR spectral diagnostics to study these cool stellar populations based on high-resolution spectroscopy is still in its pioneering stage. Any effort to make progress in the field is innovative and of impact on stellar archaeology and stellar evolution. This PhD project takes the challenge of exploring that new parameter space and characterizing the physical properties, the chemical content and the kinematics of cool giants and supergiants in selected disc fields and clusters of our Galaxy, with the ultimate goal of tracing their past and recent star formation and chemical enrichment history. By using optical HARPS-N and near-infrared GIANO-B high-resolution stellar spectra in the context of the large program SPA-Stellar Population Astrophysics: the detailed, age-resolved chemistry of the Milky Way disk” (PI L. Origlia), an extensive study of Arcturus, a standard calibrator for red giant stars, has been performed. New diagnostics of stellar parameters as well as optimal linelists for chemical analysis have been provided. Then, such diagnostics have been used to determine evolutionary properties, detailed chemical abundances of almost 30 different elements and mixing processes of a homogeneous sample of red supergiant stars in the Perseus complex.