Nous étudions la formation d’étoiles et d’amas d’étoiles dans les galaxies dominées par le gaz. Ce terme réfère en premier lieu aux galaxies de l’époque du pic de formation d’étoiles dans l’histoire de l’Univers, qui s’est déroulé vers z ~ 2, mais aussi à leurs analogues locaux, les galaxies naines de marées. En premier lieu, en utilisant des simulations numériques, nous montrons que les galaxies massives typiques de z=2, avec une fraction de gaz d’environ 50%, forment des structures gazeuses massives (10**7-8 masses solaires) et liées gravitationnellement, appelées grumeaux dans la suite. Ces grumeaux ne se forment dans des galaxies avec une fraction de gaz inférieure à 25%. Nous présentons ensuite une étude observationnelle d’un analogue local de grumeaux de galaxies à z=2, la galaxie naine de marée NGC 5291N. Une analyse des raies d’émission de cette galaxie montre la présence de chocs sur les pourtours de l’objet. La photométrie des amas d’étoiles de cette galaxie montre que les amas les plus jeunes (< 10 millions d’années) sont significativement moins massifs que les amas plus âgés. Ceci peut être le signe de fusions progressives d’amas et/ou d’une forte activité de formation stellaire dans ce système il y a environ 500 millions d’années.Dans un second lieu nous étudions comment la fraction de gaz influe sur la formation d’étoiles et d’amas stellaires dans des fusions de galaxies à z=2. En utilisant des simulations numériques nous montrons que ces fusions n’augmentent que relativement peu le taux de formation d’étoiles et d’amas stellaires comparativement aux fusions de galaxies locales, à faible fraction de gaz. Nous montrons que ceci est due à une saturation de plusieurs facteurs physiques, qui sont déjà présents naturellement dans les galaxies isolées à z=2 et sont donc comparativement peu accentués par les fusions. Il s’agit de la turbulence du gaz, des zones de champ de marée compressif et des flux de matières vers le noyau de la galaxie. Nous montrons aussi que les structures stellaires formées au sein des grumeaux de gaz sont préservées par la fusion : elles sont éjectées des disques et orbitent dans le halo de la galaxie résultante de la fusion, où elles peuvent devenir les progéniteurs de certains amas globulaires / We study the formation of stars and stellar clusters in gas-dominated galaxies. This term primarily refers to galaxies from the epoch of the peak of the cosmic star formation history, which occurred at z ~ 2, but also to their local analogues, the tidal dwarf galaxies.Firstly, using numerical simulations, we show that the massive galaxies at z = 2, which have a gas fraction of about 50%, form massive (10**7-8 solar masses) and gravitationally bound structures, which we call clumps thereafter. These clumps do not form in galaxies with a gas fraction below 25%. We then present an observational study of a local analogue of a z = 2 galactic clump, which is the tidal dwarf galaxy NGC 5291N. The analysis of emission lines show the presence of shocks on the outskirts of the object. Photometry of this galaxy’s stellar clusters show that the youngest clusters (< 10 million years) are significantly less massive than older clusters. This could be the sign of ongoing cluster mergers and/or of a strong star formation activity in this system about 500 million years ago).Secondly, we study how the gas fraction impacts the formation of stars and stellar clusters in galaxy mergers at z = 2. Using numerical simulations we show that these mergers only slightly increase the star and stellar cluster formation rate, compared to local galaxy mergers, which have a lower gas fraction. We show that this is due to the saturation of several physical quantities, which are already strong in isolated z=2 galaxies and are thus less enhanced by the merger. These factors are gas turbulence, compressive tides and nuclear gas inflows, We also show that the stellar structures formed in the gaseous clumps are preserved by the fusion: they are ejected from the disk and orbit in the halo of the remnant galaxy, where they may become the progenitors of some globular clusters

Dark matter (DM), whose nature and interaction mechanisms are still an open issue, constitutes about 25 % of the Universe energy density. Weakly Interacting Massive Particles (WIMPs) are considered as strong candidates for particle DM and their search is conveniently carried out through the detection of gamma rays. The newly discovered ultra-faint dwarf spheroidal galaxies (dSphs), located in the vicinity of the Galaxy, exhibit high values of the mass to luminosity ratio, and are therefore considered as strongly dominated by DM. These objects are within reach of the Cherenkov Telescope Array (CTA), which is the future project for gamma-ray astronomy, with an better sensitivity (one order of magnitude) with respect to the current generation experiments. The main goal of the present work is the study of the sensitivity of CTA to WIMPs DM particles, by simulating the observation of the ultra-faint dwarf spherical galaxies Triangulum II, Reticulum II and Carina III, as well as of the classical dwarf galaxy Sculptor, for different annihilation channels, between 70 GeV and 100 TeV. The sensitivity curve in the WIMPs parameter space (velocity-averaged annihilation cross section < &sigma; &nu; > and DM mass mDM) was computed. We found that, within the sample of dwarf galaxies tested, Triangulum II is the most promising source, able to reach the thermal freeze-out values in the annihilation channel &tau;+&tau;- for only 50 hours of observation. Our result, the first estimation of the sensitivity for DM searches in ultra-faint dwarfs with CTA, is consistent with results from current generation experiments, showing better performance over an extended energy range. The limited sample of available stars in the targets induces uncertainties on the DM content. Future measurements, leading to a better understanding of the sources dynamic equilibrium, can improve this situation. Even so, the combination of the high DM content in the ultra-faint dwarf galaxies, together with the excellent expected performance of the future CTA, provides a promising result for indirect DM searches. / A matéria escura, cuja natureza e mecanismos de interação ainda estão em aberto, compõe 25% da densidade de energia do Universo. Weakly Interacting Massive Particles (WIMPs) apresentam-se como forte candidatas e sua busca é convenientemente conduzida através de raios gama. As recém descobertas galáxias esferoidais anãs ultra-fracas, situadas nos arredores da Galáxia, apresentam altos valores da razão entre massa e luminosidade, sendo portanto consideradas objetos fortemente dominados por matéria escura. Esses objetos estão ao alcance do Cherenkov Telescope Array (CTA), que é o futuro projeto da astronomia gama, com sensibilidade de uma order de grandeza melhor do que os experimentos atuais. O presente trabalho teve como objetivo estudar o potencial de detecção indireta de WIMPs através de raios gama com o futuro observatório CTA, observando as galáxias esferoidais anãs ultra-fracas Triangulum II, Retículum II e Carina III e a galáxia anã clássica Sculptor, para diferentes canais de aniquilação, entre 70 GeV e 100 TeV. A curva de sensibilidade no espaço de parâmetros livres de WIMPs (massa da partícula mDM e médida da seção de choque de aniquilação ponderada pela velocidade < &sigma; &nu; >) foi calculada. Nós encontramos que dentro da amostra de galáxias anãs testadas, Triangulum II é a fonte mais promissora, capaz de testar os valores térmicos no canal de aniquilação &tau;+&tau;- considerando apenas 50 horas de observação pelo CTA. Nosso resultado, a primeira estimativa da sensibilidade para busca de matéria escura em galáxias esferoidais anãs ultra-fracas com CTA, é consistente com resultados de experimentos da geração atual, e mostra um melhor desempenho em uma faixa de energia estendida. Os resultados são afetados pelas incertezas devido à pequena amostra de estrelas dos alvos escolhidos, que se reflete no conhecimento do conteúdo de matéria escura. Novas medidas podem ajudar a esclarecer essa situação. Ainda assim, a combinação de galáxias anãs ultra-fracas, aliada às melhorias do futuro CTA, apresenta-se como um passo muito promissor para buscas indiretas de matéria escura.

6 pp. / Training and pruning newly-planted deciduous fruit trees is one of the most important steps in developing trees with a strong framework (scaffold branches). Trees with a good framework of branches can support heavy crops without limb breakage and will help to bring the young tree into production at an early age. Selection and arrangement of these branches determines the type of development and growth in later years. The goal of pruning and training is to balance vegetative and fruiting wood growth.

Diss. (sammanfattning) Uppsala : Sveriges lantbruksuniv., 2006. / Härtill 4 uppsatser.

Stars form inside clouds of molecular gas and dust. In the early stages of stellar evolution the remainders of the initial cloud form a circumstellar disk. For the next few million years the disk will slowly dissipate via accretion, outflows, photoevaporation and planet growth while the star makes its way onto the Main Sequence. This stage of a star's life is referred to as the T Tauri phase and is characterised by high-level spectrophotometric variability. This thesis aims to study and map out the environments of T Tauri stars down to the very low mass regime by the means of time-domain monitoring. Different physical processes in the system manifest themselves as variability on different time- scales as well as produce characteristic spectroscopic and photometric features at various wave- lengths. In order to study young stellar objects in depth, the observing campaigns presented in this work were designed to cover a large range of time-scales - minutes, hours, days and months. Combining all the data, this thesis establishes a baseline of over a decade for some objects. The observations also cover a wide range of wavelengths from the optical to the mid-infrared part of the spectrum. The star RW Aur experienced two long-lasting dimming events in 2010 and 2014. This thesis presents a large collection of spectral and photometric measurements carried out just before and during the 2014 event. Spectral accretion signatures indicate no change in the accretion activity of the system. Photometry indicates that parallel to the dimming in the optical the star becomes brighter in the mid-infrared. The observations in this work combined with literature data suggest that the origin of the 2014 event is most likely obscuration of the star by hot dust from the disk being lifted into the disk wind. Very low mass stars (< 0.4 M⊙) are the most common type of star in the Galaxy. In order to understand the early stages of stellar evolution we must study young very low mass stars. This work investigates the photometric and spectroscopic variability of seven brown dwarfs in star forming regions near σ Ori and ε Ori. All targets exhibit optical photometric variability between from 0.1 to over 1.0 magnitude that persists on a time-scale of at least one decade. Despite the photometric variability no change in the spectral type is measured. In the cases where the stars are accreting, modelling of the spectral changes suggest the accretion flow is more homogeneous and less funnelled compared to Sun-like T Tauri stars. The non-accreting variables are more plausibly explained by obscuration by circumstellar material, possibly a ring made out of multiple clouds of dust grains and pebbles with varying optical depths. The star-disk systems studied in this thesis have some broader implications for star and planet formation theory. The case-study of RW Aur has unambiguously demonstrated that the planet- forming environment is very dynamic and can change dramatically on short time-scales, which in turn would have implications for the diversity of planetary systems found in the Galaxy. The Orion stars have shown that the current theory for the T Tauri stage of stellar evolution is valid down to the very low mass regime. The seven dwarfs are a good example for the evolutionary path of circumstellar disks, showing the transition from gas-high, flared accretion disks (σ Ori) to dust-dominated, depleted, structured debris disks (ε Ori).

Orientador: Luiz Claudio Di Stasi / Resumo: A Doença Inflamatória Intestinal (DII) é uma doença inflamatória crônica e idiopática do intestino que inclui duas doenças distintas: a Doença de Crohn e a Retocolite Ulcerativa. Os pacientes acometidos pela DII podem sofrer de dor abdominal, diarreia e de outros sintomas socialmente inaceitáveis que comprometem sua qualidade de vida. Embora exista uma grande quantidade de fármacos destinados ao tratamento da DII, fatores como o alto custo de aquisição, os efeitos colaterais e o fato de uma parte dos pacientes não responderem inicialmente ao tratamento, têm despertado o interesse de pesquisadores na busca de novas abordagens de tratamento para a doença. Uma das alternativas é a utilização de produtos naturais com propriedades antioxidante e/ou imunomoduladora, assim como de produtos que possam modular a microbiota intestinal, prevenindo recidivas ou complementando o tratamento de pacientes acometidos pela DII. Com base nisso, estudos realizados por nosso grupo de pesquisa com a farinha de banana nanica verde (Musa sp AAA) demonstraram que a espécie apresentou um efeito anti-inflamatório intestinal. Considerando a similaridade química, a espécie Musa sp AAB (banana prata) foi selecionada para a realização do presente estudo. As bananas são ricas em fibras, amido resistente e fenóis, além de apresentarem alto valor nutricional por serem excelentes fontes de potássio, cálcio, fósforo e vitaminas A, B e C. De forma geral, as bananas apresentam atividades antidiarreica, antiulcero... (Resumo completo, clicar acesso eletrônico abaixo) / Abstract: Inflammatory bowel disease (IBD) is a chronic and idiopathic inflammation of gastrointestinal tract that comprises two major disorders: Crohn's Disease and Ulcerative Colitis. Patients affected by IBD may suffer abdominal pain, diarrhea and other socially unacceptable symptoms that compromise their quality of life. Although there are a large number of drugs for the treatment of IBD, factors such as the high cost of acquisition, side effects and the fact that many patients do not respond initially to the available treatment, have aroused the interest of researchers to evaluate new therapeutic approaches to disease. One of these alternatives is the use of natural products with antioxidant and/or immunomodulatory properties, as well as products which can modulate the intestinal microbiota, preventing relapses or complementing patient treatments. Based on this, our research group conducted studies with green dwarf banana flour (Musa sp AAA) and demonstrated its intestinal anti-inflammatory effect. Bananas are rich in fiber, resistant starch and phenols, and have high nutritional value as they are excellent sources of potassium, calcium, phosphorus and vitamins A, B and C. Generally, bananas present antidiarrheal, antiulcerogenic, antimicrobial, hypoglycemic, antihypertensive, antihypertensive and diuretic activities. Indeed, Musa sp AAA variety increased the production of SCFAs probably because they produce prebiotic effects due to the presence of fibers and resistant starch in i... (Complete abstract click electronic access below) / Mestre

De nombreuses observations astrophysiques indiquent l'existence de grandes quantités de masse manquante dans l'Univers, et ce de l'échelle galactique à l'échelle cosmologique. Découvrir la nature de cette masse invisible constitue le problème de la matière noire, qui apparaît comme l'un des enjeux majeurs de la physique moderne. Cette thèse s'inscrit dans le contexte de la détection indirecte de matière noire. Cette dernière serait composée de nouvelles particules élémentaires, dont les produits d'annihilation pourraient être observés dans le rayonnement cosmique. Nous étudions dans ce travail deux des canaux de recherche les plus prometteurs : les photons gamma et les anti-noyaux.Les objets astrophysiques permettant de placer les meilleures contraintes actuelles en rayons gamma sont les galaxies naines sphéroïdes (dSphs) de la Voie Lactée. La première partie de notre travail a été consacrée à contraindre les facteurs J d'annihilation de ces objets, qui quantifient l'amplitude des flux gamma attendus. Nous avons pour cela mis au point une configuration optimisée d'analyse de Jeans, pour reconstruire les profils de densité de matière noire et leurs incertitudes à l'aide des données cinématiques stellaires. Notre configuration a été obtenue à l'aide de tests systématiques sur de très nombreuses dSphs simulées, et nous l'avons appliquée à vingt-trois dSphs de la Voie Lactée. La seconde partie de notre travail a consisté à mener une recherche de noyaux d'anti-hélium dans les données collectées par l'expérience AMS-02 sur la Station Spatiale Internationale. Nous avons pour cela mis au point une classification par arbres de décision boostés, et notre analyse préliminaire a permis d'obtenir les meilleures contraintes actuelles sur les rapports anti-hélium sur hélium. / Many astrophysical observations suggest the existence of large amounts of missing mass in the Universe, from the galactic to the cosmological scale. Discovering the nature of this invisible mass forms the dark matter problem, which appears as one of the major challenges of modern physics. This thesis is established in the context of indirect detection of dark matter. The latter could consist of new elementary particles, whose annihilation products may be observed in cosmic rays. We study in this work two of the most promising research channels!: gamma-rays and anti-nuclei.The best constraints on dark matter properties from gamma-ray observations come from the dwarf spheroidal galaxies (dSphs) of the Milky Way. The first part of our work was devoted to computing the annihilation J-factors of these objects, which quantify the magnitude of the expected gamma-ray flux. We have developed an optimized Jeans analysis setup in order to reconstruct the dark matter density profiles of these objects and their associated uncertainties, using stellar kinematic data. Our optimized setup was obtained using systematic tests on numerous simulated dSphs, and we applied it to twenty-three dSphs of the Milky Way. The second part of our work was dedicated to the search for anti-helium nuclei in the cosmic ray data collected by the AMS-02 experiment on the International Space Station. We have developed a classification method using boosted decision trees, and our preliminary analysis has led to the best constraints to date on the anti-helium to helium ratio.

The main aim of this master thesis was the simultaneous detection of four selected plant viruses ? Apple mosaic virus, Plum pox virus, Prunus necrotic ringspot virus and Prune harf virus, by microarrays. The intermediate step in the process of the detection was optimizing of multiplex polymerase chain reaction (PCR).

abstract: The increased number of novel pathogens that potentially threaten the human population has motivated the development of mathematical and computational modeling approaches for forecasting epidemic impact and understanding key environmental characteristics that influence the spread of diseases. Yet, in the case that substantial uncertainty surrounds the transmission process during a rapidly developing infectious disease outbreak, complex mechanistic models may be too difficult to be calibrated quick enough for policy makers to make informed decisions. Simple phenomenological models that rely on a small number of parameters can provide an initial platform for assessing the epidemic trajectory, estimating the reproduction number and quantifying the disease burden from the early epidemic phase. Chapter 1 provides background information and motivation for infectious disease forecasting and outlines the rest of the thesis. In chapter 2, logistic patch models are used to assess and forecast the 2013-2015 West Africa Zaire ebolavirus epidemic. In particular, this chapter is concerned with comparing and contrasting the effects that spatial heterogeneity has on the forecasting performance of the cumulative infected case counts reported during the epidemic. In chapter 3, two simple phenomenological models inspired from population biology are used to assess the Research and Policy for Infectious Disease Dynamics (RAPIDD) Ebola Challenge; a simulated epidemic that generated 4 infectious disease scenarios. Because of the nature of the synthetically generated data, model predictions are compared to exact epidemiological quantities used in the simulation. In chapter 4, these models are applied to the 1904 Plague epidemic that occurred in Bombay. This chapter provides evidence that these simple models may be applicable to infectious diseases no matter the disease transmission mechanism. Chapter 5, uses the patch models from chapter 2 to explore how migration in the 1904 Plague epidemic changes the final epidemic size. The final chapter is an interdisciplinary project concerning within-host dynamics of cereal yellow dwarf virus-RPV, a plant pathogen from a virus group that infects over 150 grass species. Motivated by environmental nutrient enrichment due to anthropological activities, mathematical models are employed to investigate the relevance of resource competition to pathogen and host dynamics. / Dissertation/Thesis / Doctoral Dissertation Applied Mathematics 2016

Submitted by Deyse Queiroz (deysequeirozz@hotmail.com) on 2018-05-22T17:40:42Z No. of bitstreams: 1 ERBIA BRESSIA GONÇALVES ARAÚJO - DISSERTAÇÃO PPGHT - 2017.pdf: 1383874 bytes, checksum: b5f572bb8228fa61951814df473903f2 (MD5) / Made available in DSpace on 2018-05-22T17:40:42Z (GMT). No. of bitstreams: 1 ERBIA BRESSIA GONÇALVES ARAÚJO - DISSERTAÇÃO PPGHT - 2017.pdf: 1383874 bytes, checksum: b5f572bb8228fa61951814df473903f2 (MD5) Previous issue date: 2017-08-16 / No Brasil, a maioria dos pomares de cajueiro está localizada no tropico semiárido, onde os recursos hídricos são escassos e apresentam problemas de salinidade. Diante da importância socioeconômica do cajueiro para região nordeste do Brasil bem como das dificuldades relacionadas a escassez hídrica e qualidade de agua para irrigação, objetivou-se com este trabalho avaliar os efeitos da utilização de diferentes doses de matéria orgânica combinadas com águas de distintos níveis salinos na produção de porta-enxerto de cajueiro. O experimento foi desenvolvido em casa de vegetação (ambiente protegido) do Centro de Ciências e Tecnologia Agroalimentar da Universidade Federal de Campina Grande (CCTA/UFCG), localizado no município de Pombal-PB. O delineamento experimental foi em blocos casualizados, num esquema fatorial 5 x 4, com os tratamentos referentes à cinco níveis de condutividade elétrica da água de irrigação CEa de (0,3; 1,0; 1,7; 2,4 e 3,1 dS m-1 ) em interação com quatro doses matéria orgânica MO (2,5; 3,5; 4,5 e 5,5%). Utilizaram-se três repetições, com duas plantas úteis por parcela, onde se avaliou o clone de cajueiro anão precoce CCP 06. Foram avaliadas as variáveis de diâmetro do caule, número de folhas e área foliar aos 20 e 30 dias após a aplicação dos tratamentos (DAT), taxa de crescimento absoluto e relativo da altura de planta e do diâmetro do caule nos períodos de 10 a 30 DAT, fitomassa fresca e seca de caule, folhas e parte aérea, fitomassa seca de raiz, seca total e o índice de qualidade de Dickson aos 30 DAT. As doses crescentes de matéria orgânica não atenuaram o efeito da salinidade da água de irrigação sobre as variáveis estudadas no presente trabalho. A transpiração, condutância estomática e a fotossíntese líquida dos porta-enxerto de cajueiro CCP 06 diminuem com o acréscimo da salinidade do extrato de saturação do solo.Doses crescentes de MO não reduzem o efeito deletério da irrigação com águas salinizadas sobre a fitomassa e a fisiologia de portaenxerto de cajueiro CCP 06. A irrigação de água CEa de até 2,49, 0,90 e 1,01 dS m-1 , na produção de porta-enxerto de cajueiro CCP 06 promove redução aceitável no crescimento (diâmetro, área foliar e TCRap), fisiologia e fitomassa aos 30 DAT de 10% respectivamente. A dose de matéria orgânica de 2,5% apresentou o melhor resultado para as variáveis estudadas. / In Brazil, most of the cashew orchards are located in the semi-arid tropics, where water resources are scarce and present salinity problems. In view of the socioeconomic importance of cashew trees in the northeastern region of Brazil, as well as the difficulties related to water scarcity and water quality for irrigation, the objective of this work was to evaluate the effects of the use of different doses of organic matter combined with waters of different saline levels In the production of cashew rootstock. The experiment was carried out in a greenhouse (protected environment) of the Center for Science and Technology Agro-Food of the Federal University of Campina Grande (CCTA / UFCG), located in the municipality of Pombal-PB. The experimental design was a randomized complete block design, in a 5 x 4 factorial scheme, with the treatments referring to five levels of electrical conductivity of ECw irrigation water of (0.3, 1.0, 1.7, 2.4 and 3, 1 dS m-1 ) in interaction with four organic matter doses OM (2.5, 3.5, 4.5 and 5.5%). Three replicates were used, with two useful plants per plot, where the precocious dwarf cashew clone CCP 06 was evaluated. The variables of stem diameter, number of leaves and leaf area were evaluated at 20 and 30 days after application of the treatments (DAT), absolute and relative growth rate of plant height and stem diameter in periods of 10 to 30 DAT, fresh and dry stem, leaf and shoot biomass, dry root phytomass, total dry matter and Quality of Dickson at 30 DAT. Increasing doses of organic matter did not attenuate the effect of irrigation water salinity on the variables studied in the present study. The transpiration, stomatal conductance and the net photosynthesis of the CCP 06 cashew rootstocks decrease with the increase of the salinity of the soil saturation extract. Increasing OM masses do not reduce the deleterious effect of irrigation with salinized waters on phytomass and physiology Of CCP 06 cashew tree rootstock. ECw water irrigation of up to 2.49, 0.90 and 1.01 dS m-1 in the production of CCP 06 cashew rootstock promotes acceptable growth reduction (diameter, Leaf area and TCRap), physiology and phytomass at 30 DAT of 10%, respectively. The organic matter dose of 2.5% presented the best results for the studied variables.