Offshore wind resource estimation using wave buoy data

In the coming decade installed offshore wind capacity is expected to expand rapidly. This will be both technically and economically challenging. Precise wind resource assessment is one of the more imminent challenges. It is more difficult to assess wind power offshore than onshore due to the paucity of representative wind speed data. Offshore site-specific data is less accessible and is far more costly to collect. However, offshore wind speed data collected from sources such as wave buoys, remote sensing from satellites, national weather ships, and coastal meteorological stations and met masts on barges and platforms may be extrapolated to assess offshore wind power. This study attempts to determine the usefulness of pre-existing offshore wind speed measurements in resource assessment, and presents the results of wind resource estimation in the Atlantic Ocean and in the Irish Sea using data from two offshore meteorological buoys. © 2012 IEEE.

Characteristics of Offshore Wind Speeds using Buoy Measurements

In the coming decade installed offshore wind capacity is expected to expand rapidly. This will be both technically and economically challenging. Precise wind resource assessment is one of the more imminent challenges. It is more difficult to assess wind power offshore than onshore due to the paucity of representative wind speed data. Offshore site-specific data is less accessible and is far more costly to collect. However, offshore wind speed data collected from sources such as wave buoys, remote sensing from satellites, national weather ships, and coastal meteorological stations and met masts on barges and platforms may be extrapolated to assess offshore wind power. This study attempts to determine the usefulness of pre-existing offshore wind speed measurements in resource assessment, and presents the results of wind resource estimation in the Atlantic Ocean and in the Irish Sea using data from two offshore meteorological buoys

Magnetospheric Structure and Atmospheric Joule Heating of Habitable Planets Orbiting M-dwarf Stars

We study the magnetospheric structure and the ionospheric Joule Heating of planets orbiting M-dwarf stars in the habitable zone using a set of magnetohydrodynamic models. The stellar wind solution is used to drive a model for the planetary magnetosphere, which is coupled with a model for the planetary ionosphere. Our simulations reveal that the space environment around close-in habitable planets is extreme, and the stellar wind plasma conditions change from sub- to super-Alfvénic along the planetary orbit. As a result, the magnetospheric structure changes dramatically with a bow shock forming in the super-Alfvénic sectors, while no bow shock forms in the sub-Alfvénic sectors. The planets reside most of the time in the sub-Alfvénic sectors with poor atmospheric protection. A significant amount of Joule Heating is provided at the top of the atmosphere as a result of the intense stellar wind. For the steady-state solution, the heating is about 0.1%-3% of the total incoming stellar irradiation, and it is enhanced by 50% for the time-dependent case. The significant Joule Heating obtained here should be considered in models for the atmospheres of habitable planets in terms of the thickness of the atmosphere, the top-side temperature and density, the boundary conditions for the atmospheric pressure, and particle radiation and transport. Here we assume constant ionospheric Pedersen conductance similar to that of the Earth. The conductance could be greater due to the intense EUV radiation leading to smaller heating rates. We plan to quantify the ionospheric conductance in future study.

The high-energy environment in the super-Earth system CoRoT-7

High-energy irradiation of exoplanets has been identified to be a key influence on the stability of these planets' atmospheres. So far, irradiation-driven mass-loss has been observed only in two Hot Jupiters, and the observational data remain even more sparse in the super-Earth regime. We present an investigation of the high-energy emission in the CoRoT-7 system, which hosts the first known transiting super-Earth. To characterize the high-energy XUV radiation field into which the rocky planets CoRoT-7b and CoRoT-7c are immersed, we analyzed a 25 ks XMM-Newton observation of the host star. Our analysis yields the first clear (3.5σ) X-ray detection of CoRoT-7. We determine a coronal temperature of ≈ 3 MK and an X-ray luminosity of 3 × 1028 erg s-1. The level of XUV irradiation on CoRoT-7b amounts to ≈37 000 erg cm-2 s-1. Current theories for planetary evaporation can only provide an order-of-magnitude estimate for the planetary mass loss; assuming that CoRoT-7b has formed as a rocky planet, we estimate that CoRoT-7b evaporates at a rate of about 1.3 × 1011 g s-1 and has lost ≈4-10 earth masses in total.

The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems

When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Since the LOS velocities depend, in part, on the stellar rotation, the RM waveform is sensitive to the star-planet alignment (which provides information on the system’s dynamical history). We present a new RM modelling technique that directly measures the spatially-resolved stellar spectrum behind the planet. This is done by scaling the continuum flux of the (HARPS) spectra by the transit light curve, and then subtracting the infrom the out-of-transit spectra to isolate the starlight behind the planet. This technique does not assume any shape for the intrinsic local profiles. In it, we also allow for differential stellar rotation and centre-to-limb variations in the convective blueshift. We apply this technique to HD 189733 and compare to 3D magnetohydrodynamic (MHD) simulations. We reject rigid body rotation with high confidence (>99% probability), which allows us to determine the occulted stellar latitudes and measure the stellar inclination. In turn, we determine both the sky-projected (λ ≈ −0.4 ± 0.2◦) and true 3D obliquity (ψ ≈ 7+12 −4 ◦ ). We also find good agreement with the MHD simulations, with no significant centre-to-limb variations detectable in the local profiles. Hence, this technique provides a new powerful tool that can probe stellar photospheres, differential rotation, determine 3D obliquities, and remove sky-projection biases in planet migration theories. This technique can be implemented with existing instrumentation, but will become even more powerful with the next generation of high-precision radial velocity spectrographs.

Modeling the Rossiter-McLaughlin Effect: Impact of the Convective Center-to-limb Variations in the Stellar Photosphere

bservations of the Rossiter–McLaughlin (RM) effect provide information on star–planet alignments, which can inform planetary migration and evolution theories. Here, we go beyond the classical RM modeling and explore the impact of a convective blueshift that varies across the stellar disk and non-Gaussian stellar photospheric profiles. We simulated an aligned hot Jupiter with a four-day orbit about a Sun-like star and injected center-to-limb velocity (and profile shape) variations based on radiative 3D magnetohydrodynamic simulations of solar surface convection. The residuals between our modeling and classical RM modeling were dependent on the intrinsic profile width and v sin i; the amplitude of the residuals increased with increasing v sin i and with decreasing intrinsic profile width. For slowly rotating stars the center-to-limb convective variation dominated the residuals (with amplitudes of 10 s of cm s−1 to ~1 m s−1); however, for faster rotating stars the dominant residual signature was due a non-Gaussian intrinsic profile (with amplitudes from 0.5 to 9 m s−1). When the impact factor was 0, neglecting to account for the convective center-to-limb variation led to an uncertainty in the obliquity of ~10°–20°, even though the true v sin i was known. Additionally, neglecting to properly model an asymmetric intrinsic profile had a greater impact for more rapidly rotating stars (e.g., v sin i = 6 km s−1) and caused systematic errors on the order of ~20° in the measured obliquities. Hence, neglecting the impact of stellar surface convection may bias star–planet alignment measurements and consequently theories on planetary migration and evolution.

Sistemas de recepção de imagens de satélite: implementação e aplicações

A presente dissertação pretende focalizar-se sobre algumas aplicações da detecção remota por satélite. Assim, será exposto neste trabalho o resultado do desenvolvimento de sistemas de recepção de imagens obtidas por satélites de órbita polar e geostacionária, assim como um conjunto de três aplicações implementadas: a detecção de focos de incêndio em Portugal com dados do MSG-1, o desenvolvimento de um conjunto de actividades de exploração da Detecção Remota no contexto do 1' Ciclo do Ensino Básico e a validação dos resultados de previsão do modelo de mesoescala MM5 com imagens de satélite. A análise destas imagens desempenha um papel crucial, por exemplo nos estudos sobre tempo e clima. É por essa razão que tanto os Estados Unidos como outros países têm vindo a desenvolver um esforço contínuo para que possam ser lançados novos satélites que permitam uma constante aquisição de conhecimentos sobre os fenómenos meteorológicos. Deste modo, a implementação de sistemas de recepção que possibilitem transformar as medidas disponibilizadas por instrumentos a bordo de satélites em informação constitui um empreendimento de extrema utilidade para as mais diversas áreas do saber (como as Geociências ou a Meteorologia), revestindo-se de inúmeras aplicações de interesse para a Sociedade, nomeadamente nos sectores agrícola, energético, dos transportes e da conservação do meio ambiente.

Wind energy resource modelling in Portugal and its future large-scale alteration due to anthropogenic induced climate changes

The high dependence of Portugal from foreign energy sources (mainly fossil fuels), together with the international commitments assumed by Portugal and the national strategy in terms of energy policy, as well as resources sustainability and climate change issues, inevitably force Portugal to invest in its energetic self-sufficiency. The 20/20/20 Strategy defined by the European Union defines that in 2020 60% of the total electricity consumption must come from renewable energy sources. Wind energy is currently a major source of electricity generation in Portugal, producing about 23% of the national total electricity consumption in 2013. The National Energy Strategy 2020 (ENE2020), which aims to ensure the national compliance of the European Strategy 20/20/20, states that about half of this 60% target will be provided by wind energy. This work aims to implement and optimise a numerical weather prediction model in the simulation and modelling of the wind energy resource in Portugal, both in offshore and onshore areas. The numerical model optimisation consisted in the determination of which initial and boundary conditions and planetary boundary layer physical parameterizations options provide wind power flux (or energy density), wind speed and direction simulations closest to in situ measured wind data. Specifically for offshore areas, it is also intended to evaluate if the numerical model, once optimised, is able to produce power flux, wind speed and direction simulations more consistent with in situ measured data than wind measurements collected by satellites. This work also aims to study and analyse possible impacts that anthropogenic climate changes may have on the future wind energetic resource in Europe. The results show that the ECMWF reanalysis ERA-Interim are those that, among all the forcing databases currently available to drive numerical weather prediction models, allow wind power flux, wind speed and direction simulations more consistent with in situ wind measurements. It was also found that the Pleim-Xiu and ACM2 planetary boundary layer parameterizations are the ones that showed the best performance in terms of wind power flux, wind speed and direction simulations. This model optimisation allowed a significant reduction of the wind power flux, wind speed and direction simulations errors and, specifically for offshore areas, wind power flux, wind speed and direction simulations more consistent with in situ wind measurements than data obtained from satellites, which is a very valuable and interesting achievement. This work also revealed that future anthropogenic climate changes can negatively impact future European wind energy resource, due to tendencies towards a reduction in future wind speeds especially by the end of the current century and under stronger radiative forcing conditions.

Pollen Sources

This chapter reviews what is known about abundance and distribution of the 12 most important aeroallergenic pollens in Europe: Ambrosia, Alnus, Artemisia, Betula, Chenopodiaceae, Corylus, Cupressaceae/Taxaceae, Olea, Platanus, Poaceae, Quercus and Urtica/Parietaria. Abundance is based on 10 years of pollen records from 521 stations of the European Aeroallergen Network that were interpolated into 12 distribution maps covering most of Europe. The chapter compares the distribution maps with other types of distribution maps that are available for selected tree species and discuss two methods for making harmonized pollen source inventories: “bottom-up” and “top-down”. Both methods have advantages and disadvantages, and both need to be explored and further developed. Remote sensing has shown to be a valuable method to improve the inventories, especially the use of satellites. The full potential as well as limitations of remote sensing in relation to pollen sources remains to be explored. The review suggests that the most probable way of obtaining inventories of all 12 pollen species is to use top-down methods that use an ecosystem-based approach that for each particular species connects ecological preference, pollen counts and remote sensing.

Behaviour and life history of a large carpenter bee (Xylocopa virginica) in the northern extent of its range

Large carpenter bees (Hymenoptera: Apidae: Xylocopa) have traditionally been thought of as exhibiting solitary or occasionally communal colony social organization. However, studies have demonstrated more complex fonns of social behaviour in this genus. In this document, I examine elements ofbehaviour and life history in a North American species at the northern extreme of its range. Xylocopa virginica was found to be socially polymorphic with both solitary and meta-social or semi-social nests in the same population. In social nests, there is no apparent benefit from additional females which do not perfonn significant work or guarding. I found that the timing of life-history events varies between years, yet foraging effort only differed in the coldest and wettest year of2004 the study. Finally, I that male X virginica exhibit female defence polygyny, with resident and satellite males. Resident males maintain their territories through greater aggression relative to satellites.

Transposable Elements Are a Significant Contributor to Tandem Repeats in the Human Genome

Sequence repeats are an important phenomenon in the human genome, playing important roles in genomic alteration often with phenotypic consequences. The two major types of repeat elements in the human genome are tandem repeats (TRs) including microsatellites, minisatellites, and satellites and transposable elements (TEs). So far, very little has been known about the relationship between these two types of repeats. In this study, we identified TRs that are derived from TEs either based on sequence similarity or overlapping genomic positions. We then analyzed the distribution of these TRs among TE families/subfamilies. Our study shows that at least 7,276 TRs or 23% of all minisatellites/satellites is derived from TEs, contributing ∼0.32% of the human genome. TRs seem to be generated more likely from younger/more active TEs, and once initiated they are expanded with time via local duplication of the repeat units. The currently postulated mechanisms for origin of TRs can explain only 6% of all TE-derived TRs, indicating the presence of one or more yet to be identified mechanisms for the initiation of such repeats. Our result suggests that TEs are contributing to genome expansion and alteration not only by transposition but also by generating tandem repeats.

Impact de l’évolution des formes de croissance urbaine sur l’identité de la ville et de ses citoyens

L’évolution de l’urbanisation dans le monde nous a motivés à développer nos recherches quant à cette croissance déchaînée des villes et ces multitudes de formes urbaines qui en résultent. L'objet de ce travail est d'analyser ces formes de croissance spatiales et d’analyse leur impact sur l’identité dans la ville. Il s'agit de montrer dans quelle mesure elles favorisent la prolifération de nouvelles identités dans les régions périphériques de la ville. Notre recherche porte alors sur une étude socio spatiale de la capitale de la Tunisie. Tunis, cette métropole en pleine expansion, occupe un emplacement stratégique dans la Méditerranée et joue un rôle important dans les échanges afro-européens. La pertinence de l’étude de l’évolution du domaine urbain de Tunis résulte du fait que cette ville a connu différents types de croissances. La variété des modes de développement de l’espace urbain fait de Tunis un exemple pertinent qui mérite d’être étudié, d’autant plus que l’espace englobe des banlieues planifiées, spontanées, historiques, et bien d’autres qui résultent du juste fait de l’informalité, allant du patrimoine à la construction d’une identité urbaine plurielle. Notre travail comportera donc une étude spatiale de l’évolution de l’espace urbain de Tunis, basée essentiellement sur des cartes et des photos satellites, doublées d’une analyse sociale, basée sur une enquête in situ, réalisée avec les habitants des banlieues, et ce, dans le but de recenser leurs degrés d’attachement à l’espace ainsi que les rapports qu’ils entament avec le centre-ville. Notre recherche nous a permis de conclure que les habitants des banlieues s’identifient aux nouvelles formes de croissance et développent au fil des années un sentiment d’appartenance et d’attachement identitaire à leurs quartiers. Cela contribue à la prolifération d’identités multiple dans la ville.

De la réforme et de l'harmonisation du droit des sûretés dans un contexte de mondialisation de l'économie : vers un retour au paradigme de l'uniformisation du droit?

La réforme et l’harmonisation du droit des sûretés mobilières sont à l’ordre du jour de plusieurs organisations internationales, car il est admis qu’un régime de sûretés efficient favorise l’accès au crédit à de faibles coûts. L’harmonisation de ce droit comporte deux volets. D’une part, dans l’Occident industrialisé, les efforts d’harmonisation vont de la réforme des droits internes à l’établissement de régimes spéciaux relativement à des biens spécifiques (principalement les biens mobiles de grande valeur, tels les aéronefs, le matériel ferroviaire roulant et les satellites, et les biens incorporels, comprenant les créances, valeurs mobilières, actifs financiers et titres intermédiés). Ces efforts d’harmonisation démontrent que d’un point de vue systémique, malgré quelques différences notables, les régimes nord-américains et européens sont fondés sur des principes similaires et atteignent des résultats comparables. En résulte l’émergence d’un ordre juridique transnational en droit des sûretés mobilières, fondé sur les principes de la primauté de l’individu et la reconnaissance du droit de propriété de l’individu dans ses biens, mis en œuvre grâce à l’État de droit. D’autre part, les institutions financières internationales encouragent l’établissement de régimes de sûretés dans les pays en voie de développement qui obéissent aux mêmes critères que ceux de l’Occident, en insistant sur les réformes institutionnelles et juridiques visant l’établissement d’une bonne gouvernance et l’État de droit. Cependant, une transposition des régimes occidentaux ne peut se faire sans heurts dans les pays en voie de développement, notamment pour des raisons socio-culturelles et politiques. Lorsque les principes de la primauté de l’individu, de la propriété individuelle et de l’État de droit ne sont pas reconnus dans un pays donné, la réforme et l’harmonisation du droit des sûretés s’en trouvent compromis. La démonstration de l’état d’avancement de la réforme et de l’harmonisation du droit des sûretés dans les pays occidentaux industrialisés est faite grâce à une comparaison du Uniform Commercial Code, du Code civil du Québec, des Personal Property Security Acts des provinces canadiennes de common law, des principes des droits français et anglais, de l’influence du droit communautaire sur les pays membres de l’Union Européenne. Sont analysés, aussi, dans cette optique, les principaux instruments de l’harmonisation du droit émanant des organisations internationales. Par ailleurs, deux études de cas relatifs à la réforme du crédit foncier en Égypte et à la réforme de l’urbanisme et de l’habitat en République démocratique du Congo, viennent étayer les difficultés que rencontrent les institutions internationales, telles la Banque mondiale et l’ACDI, dans le cadre de projets de réformes visant la bonne gouvernance et l’instauration d’un véritable État de droit, en partie à cause d’un pluralisme des ordres juridiques de ces pays.

Détection de points chauds de déforestation à Bornéo de 2000 à 2009 à partir d'images MODIS

Ce travail s’inscrit dans le cadre d’un programme de recherches appuyé par le Conseil de recherches en sciences humaines du Canada.

Modélisation de l'irradiance solaire spectrale dans le proche et moyen ultraviolet

Nous présentons un modèle pour l’irradiance solaire spectrale entre 200 et 400 nm. Celui-ci est une extension d’un modèle d’irradiance solaire totale basé sur la simulation de la fragmentation et l’érosion des taches qui utilise, en entrée, les positions et aires des taches observées pour chaque pas de temps d’une journée. L’émergence des taches sur la face du Soleil opposée à la Terre est simulée par une injection stochastique. Le modèle simule ensuite leur désintégration, qui produit des taches plus petites et des facules. Par la suite, l’irradiance est calculée en sommant la contribution des taches, des facules et du Soleil inactif. Les paramètres libres du modèle sont ajustés en comparant les séquences temporelles produites avec les données provenant de divers satellites s’étalant sur trois cycles d’activité. Le modèle d’irradiance spectrale, quant à lui, a été obtenu en modifiant le calcul de la contribution des taches et des facules, ainsi que celle du Soleil inactif, afin de tenir compte de leur dépendance spectrale. Le flux de la photosphère inactive est interpolé sur un spectre synthétique non magnétisé, alors que le contraste des taches est obtenu en calculant le rapport du flux provenant d’un spectre synthétique représentatif des taches et de celui provenant du spectre représentatif du Soleil inactif. Le contraste des facules est quand à lui calculé avec une procédure simple d’inversion de corps noir. Cette dernière nécessite l’utilisation d’un profil de température des facules obtenu à l’aide de modèles d’atmosphère. Les données produites avec le modèle d’irradiance spectrale sont comparées aux observations de SOLSTICE sur UARS. L’accord étant peu satisfaisant, particulièrement concernant le niveau d’irradiance minimal ainsi que l’amplitude des variations, des corrections sont appliquées sur le flux du Soleil inactif, sur le profil de température des facules, ainsi qu’à la dépendance centre-bord du contraste des facules. Enfin, un profil de température des facules est reconstruit empiriquement en maximisant l’accord avec les observations grâce à un algorithme génétique. Il est utilisé afin de reconstruire les séquences temporelles d’irradiance jusqu’en 1874 à des longueurs d’ondes d’intérêt pour la chimie et la dynamique stratosphérique.