No description available.

We implement a model for, and study the effects of, AGN feedback in cosmological hydrodynamical simulations. In our model, black holes form high-density, primordial gas, to imitate the likely channels of black hole formation in the early Universe. We find that a black hole seed mass of 10²⁻³h⁻¹M⊙ is required to produce simulations that match the cosmic star formation rate density, and present-day black hole mass - velocity dispersion and galaxy size - velocity dispersion relations. We therefore suggest that Population III stars can be the progenitors of the super-massive black holes seen today. Using our fiducial model, we run two large simulations ((25h⁻¹ Mpc)³), one with and one without AGN feedback. With these, we follow the population of galaxies that forms across cosmic time, and find that the inclusion of AGN feedback improves the agreement of simulated and observed galaxy properties, such as the mass and luminosity functions. This agreement is best at z = 0, and fairly good out to z = 2-3. Evidence for downsizing in the evolution of galaxies is found, both in the present-day colour-magnitude and [α/Fe]-velocity dispersion relations, and by the fact that high-mass galaxies attain their present-day metallicity earlier and faster than do low-mass ones. With our hydrodynamical simulations, we can also investigate the internal structure of galaxies, and look at the effects of galaxy mergers and AGN feedback on the stellar and gas-phase metallicity gradients of galaxies. Stellar metallicity gradients are found to be sensitive to galaxy mergers, while gas-phase metallicity gradients are more affected by AGN activity. This suggests that simultaneous measurements of these two quantities can help disentangle the actions of mergers and AGN feedback on a galaxy's history. Finally, we develop a new method to identify massive AGN-driven outflows from the most massive simulated galaxy. These events cause the intra-cluster medium to be hotter and more chemically enriched compared to the simulation without AGN feedback, and therefore AGN feedback may be required in order to attain the metallicities observed in clusters.

Recently, experimental observations have shown that radar echoes from the irregularity<br />source region associated with mesospheric dusty space plasmas may be modulated by radio wave heating with ground-based ionospheric heating facilities. These experiments show great promise as a diagnostic for the associated dusty plasma in the Near-Earth Space Environment which is believed to have links to global change. This provides an alternative to more complicated and costly space-based observational approaches to investigating these layers. This dissertation seeks to develop new analytical and computational models to investigate fundamental physics of the associated dusty plasmas as well as utilize experimental observations during High Frequency HF ground-based heating experiments to develop practical techniques for diagnosing these dusty plasma layers.<br />The dependency of the backscattered signal strength (i.e. Polar Mesospheric Summer Echoes PMSEs) after the turn-on and turn-off of the radio wave heating on the radar frequency is an unique phenomenon that can shed light on the unresolved issues associated with the basic physics of the natural charged mesospheric dust layer. The physical process after turn-on and turn-off of radio wave heating is explained by competing ambipolar diffusion and dust charging processes. The threshold radar frequency and dust parameters for the enhancement or suppression of radar echoes after radio wave heating turn-on are investigated for measured mesospheric plasma parameters. The effect of parameters such as the electron temperature enhancement during radiowave heating, dust density, dust charge polarity, ion-neutral collision frequency, electron density and dust radius<br />on the temporal evolution of electron irregularities associated with PMSE is investigated.<br />The possibility of observing the turn-on overshoot (enhancement of radar echoes after the<br />radiowave turn-on) in the high frequency HF radar band is discussed based on typical mesospheric<br />parameters. It has been shown that predicted enhancement of electron irregularity<br />amplitude after heater turn-on at HF band is the direct manifestation of the dust charging<br />process in the space. Therefore further active experiments of PMSEs should be pursued<br />at HF band to illuminate the fundamental charging physics in the space environment to<br />provide more insight on this unique medium. Preliminary observation results of HF PMSE<br />heating experiment with the new 7.9 MHz radar at the European Incoherent Scatter EISCAT<br />facility appear promising for the existence of PMSE turn-on overshoot. Therefore, future<br />experimental campaigns are planned to validate these predictions.<br />Computational results are used to make predictions for PMSE active modification experiments at 7.9, 56, 139, 224 and 930MHz corresponding to existing ionospheric heating facilities. Data from a 2009 very high frequency VHF (224 MHz) experiment at EISCAT<br />is compared with the computational model to obtain dust parameters in the PMSE. The<br />estimated dust parameters as a result of these comparison show very reasonable agreement to dust radius and density at PMSE altitudes measured during a recent rocket experiment providing validation to the computational model.<br /><br />The first comprehensive analytical model for the temporal evolution of PMSE after heater<br />turn-on is developed and compared to a more accurate computational model as a reference.<br />It is shown that active PMSE heating experiments involving multiple observing frequencies<br />at 7.9 (HF), 56, and 224 MHz (VHF) may contribute further diagnostic capabilities since<br />the temporal evolution of radar echoes is substantially different for these frequency ranges.<br />It is shown that conducting PMSE active experiments at HF and VHF band simultaneously<br />may allow estimation of the dust density altitude profile, dust charge state variation during<br />the heating cycle, and ratio of electron temperature enhancement in the irregularity source<br />region. These theoretical and computational models are extended to study basic physics of the evolution of relevant dusty plasma instabilities thought to play an important role in irregularity production in mesospheric dust layers. A key focus is the boundary layer of these charged dust clouds. Several aspects of the cloud\'s structure (thickness of boundary layer, average particle size and density, collisional processes, and cloud expansion speed) and the ambient plasma are varied to determine the effect of these quantities on the resulting irregularities.<br />It was shown that for high collision frequencies, the waves may be very weakly excited (or<br />even quenched) and confined to the boundary layer. The excited dust acoustic waves inside<br />the dust cloud with frequency range of 7-15Hz and in the presence of electron bite-outs is<br />consistent with measured low frequency waves near 10 Hz by sounding rocket experiments<br />over the past decade. The observed radar echoes associated with the artificially created dust<br />clouds at higher altitudes in the ionosphere including space shuttle exhaust and upcoming<br />active space experiments in which localized dust layers will be created by sounding rockets<br />could be related to the excited acoustic waves predicted.<br />Finally, variation of spatial structures of plasma and dust (ice) irregularities in the PMSE<br />source region in the presence of positively charged dust particles is investigated. The correlation and anti-correlation of fluctuations in the electron and ion densities in the background plasma are studied considering the presence of positive dust particle formation. Recent rocket payloads have studied the properties of aerosol particles within the ambient plasma environment in the polar mesopause region and measured the signature of the positively charged particles with number densities of (2000 cm"3) for particles of 0.5-1 nm in radius.<br />The measurement of significant numbers of positively charged aerosol particles is unexpected from the standard theory of aerosol charging in plasma. Nucleation on the cluster ions is one of the most probable hypotheses for the positive charge on the smallest particles. The utility being that it may provide a test for determining the presence of positive dust particles.<br />The results of the model described show good agreement with observed rocket data. As an<br />application, the model is also applied to investigate the electron irregularity behavior during<br />radiowave heating assuming the presence of positive dust particles. It is shown that the<br />positive dust produces important changes in the behavior during Polar Mesospheric Summer Echo PMSE heating experiments that can be described by the fluctuation correlation and anti-correlation properties.<br />The second part of this dissertation is dedicated to Stimulated Electromagnetic Emissions SEEs produced by interaction of high power electromagnetic waves in the ionosphere. Nearearth ionospheric plasma presets a neutral laboratory for investigation of nonlinear wave phenomena in plasma which can not be studied in the laboratory environment due to the effect of physical boundary conditions. This process has been of great interest due to the<br />important diagnostic possibilities involving ability to determine mass of constitutive ions in<br />the interaction region through measurements of various gyro-frequencies. Objectives include<br />the consideration of the variation of the spectral behavior under pump power, proximity to<br />the gyro-harmonic frequency, and beam angle. Also, the relationship between such spectral<br />features and electron acceleration and creation of plasma irregularities was an important<br />focus.<br />Secondary electromagnetic waves excited by high power electromagnetic waves transmitted<br />into the ionosphere, commonly know as Stimulated Electromagnetic Emissions SEEs,<br />produced through Magnetized Stimulated Brillouin Scatter MSBS are investigated. Data<br />from two recent research campaigns at the High Frequency Active Auroral Research Program<br />facility HAARP is presented in this work. These experiments have provided additional<br />quantitative interpretation of the SEE spectrum produced by MSBS to yield diagnostic measurements of the electron temperature in the heated ionosphere. SEE spectral emission lines corresponding to ion acoustic IA and electrostatic ion cyclotron EIC modes were observed with a shift in frequency up to a few tens of Hz from radio waves transmitted near the third harmonic of the electron gyro-frequency 3fce. The threshold of each emission line has been measured by changing the pump wave amplitude. The experimental results aimed to show the threshold for transmitter power to excite IA waves propagating along the magnetic field lines as well as for EIC waves excited at oblique angles relative to the background magnetic field. A full wave solution has been used to estimate the amplitude of the electric field at the interaction altitude. The estimated growth rate using the theoretical model is compared with the threshold of MSBS lines in the experiment and possible diagnostic information for the background ionospheric plasmas is discussed. Simultaneous formation of artificial field aligned irregularities FAIs and suppression of the MSBS process is investigated. Recently, there has been significant interest in ion gyro-harmonic structuring the Stimulated Electromagnetic Emission SEE spectrum due to the potential for new diagnostic information available about the heated volume and ancillary processes such as creation of artificial ionization layers. These relatively recently discovered emission lines have almost exclusively been studied for second electron gyro-harmonic heating. The first extensive systematic investigations of the possibility of these spectral features for third electron gyro-harmonic heating are provided here. Discrete spectral features shifted from the transmit frequency ordered by harmonics of the ion gyro-frequency were observed for third electron gyro-harmonic heating for the first time at a recent campaign at a High Frequency Active Auroral Research Program Facility HAARP. These features were also closely correlated with a broader band feature at a larger frequency shift from the transmit frequency known as the Downshifted Peak DP. The power threshold of these spectral features was measured, as well as their behavior with heater<br />beam angle, and proximity of the transmit frequency to the third electron gyro-harmonic frequency. Comparisons were also made with similar spectral features observed during 2nd<br />electron gyro-harmonic heating during the same campaign. A theoretical model is provided<br />that interprets these spectral features as resulting from parametric decay instabilities in<br />which the pump field ultimately decays into high frequency upper hybrid/electron Bernstein<br />and low frequency neutralized ion Bernstein IB and/or obliquely propagating ion acoustic<br />waves at the upper hybrid interaction altitude. Coordinated optical and SEE observations<br />were carried out in order to provide a better understanding of electron acceleration and precipitation<br />processes. Optical emissions were observed associated with SEE gyro-harmonic<br />features for pump heating near the second electron gyro-harmonic during the campaign. The<br />observations affirm strong correlation between the gyro-structures and the airglow. / Ph. D.

No description available.

This thesis presents results from two simulation studies of galaxy formation. In the first project, a dark-matter-only HORIZON simulation is used to investigate the environment and redshift dependence of mass accretion onto haloes and subhaloes. It is found that the halo accretion rate varies less strongly with redshift than predicted by the Extended Press--Schechter formalism, and that low accretion events may drive the radio-mode feedback hypothesized for recent galaxy formation models. The subhaloes at $z<0.5$ in the simulation accrete at higher rates than haloes, on average, and it is argued that this is due to their enhanced clustering at small scales. There is no dependence of accretion rate on environment at $zsim2$, but a weak correlation emerges at $zleq0.5$. The results further support previous suggestions that at $z>1$, dark matter haloes and their associated black holes grew coevally, but imply that haloes could be accreting at fractional rates that are up to a factor of 3--4 higher than their associated black holes by the present day. In the second project, outputs from one of the Adaptive Mesh Refinement NUT simulations are analyzed in order to test whether filamentary flows of cold gas are responsible for the build-up of angular momentum within a Milky Way type disk at $zgeq3$. A set of algorithms are presented that use the resolved physical scale of $12,mathrm{pc}$ to identify: (i) the central gas disk and its plane of orientation; (ii) the complex individual filament trajectories that connect to the disk, and; (iii) the infalling satellites. The results suggest that two filaments at $zgtrsim 5.5$, which later merge to form a single filament at $zlesssim 4$, drive the angular momentum and mass budget of the disk between $3lesssim zlesssim 8$, whereas luminous satellite mergers make negligible fractional contributions. These findings hence provide strong quantitative evidence that the growth of thin disks in low mass haloes at high redshift is supported via inflowing streams of cold gas.

No presente trabalho estudamos a difusão de compostos dispersos atmosfericamente como, por exemplo, fertilizantes e pesticidas particulares, em ambientes agrícolas de larga escala. Tal estudo foca-se na aplicabilidade de modelos numéricos e teórico-fenomenológicos de fenômenos turbulentos em estimativas de vantagens econômica e ambiental desses sistemas. A atmosfera terrestre, em escalas de tamanho e velocidade típicas do objeto de estudo deste trabalho, é um sistema turbulento. A turbulência é um fenômeno complexo, que envolve a interação dinâmica de distintas escalas resultando em um efeito coletivo de larga escala, decorrente de uma interação não linear entre modos perturbativos em um fluido. A modelagem da turbulência, portanto, é em geral possível através de Simulação Numérica Direta - DNS (Direct Numeric Simulation). Uma das consequências típicas da turbulência é a difusão, ou seja, o aumento em sistemas abertos da separação entre corpos particulados, em taxas muito superiores àquelas da difusão molecular térmica padrão. Neste trabalho, apresentamos um estudo focado na quantificação da difusão turbulenta de partículas através de simulações numéricas de turbulência, com o objetivo de identificar impactos de fertilização e dispersão de poluentes atmosféricos com implicações na saúde e ambiente / In the present study, we study the diffusion dispersed atmospherically compounds, such as fertilizers and particular pesticides in large scale agricultural environments. This study focuses on the applicability of numerical and theoretical and phenomenological models of turbulent phenomena in estimates of economic and environmental advantages of these systems. The Earth\'s atmosphere, in typical size and speed ranges of the study object of this work is a turbulent system. Turbulence is a complex phenomenon which involves the dynamic interaction of different ranges resulting in a large-scale collective effect due to a nonlinear interaction between perturbation modes in a fluid. The modeling of turbulence, so it is generally possible through Direct Numerical Simulation - DNS. A typical consequence of turbulence is the diffusion, i.e., increased separation in unbound systems of particulate bodies, much higher than those of the standard thermal molecular diffusion rates. In this work we present a study focused on quantifying the turbulent diffusion of particles through numerical simulations of turbulent media, in order to identify the impact of fertilization and dispersion of air pollutants on human health and environment

No presente trabalho estudamos a difusão de compostos dispersos atmosfericamente como, por exemplo, fertilizantes e pesticidas particulares, em ambientes agrícolas de larga escala. Tal estudo foca-se na aplicabilidade de modelos numéricos e teórico-fenomenológicos de fenômenos turbulentos em estimativas de vantagens econômica e ambiental desses sistemas. A atmosfera terrestre, em escalas de tamanho e velocidade típicas do objeto de estudo deste trabalho, é um sistema turbulento. A turbulência é um fenômeno complexo, que envolve a interação dinâmica de distintas escalas resultando em um efeito coletivo de larga escala, decorrente de uma interação não linear entre modos perturbativos em um fluido. A modelagem da turbulência, portanto, é em geral possível através de Simulação Numérica Direta - DNS (Direct Numeric Simulation). Uma das consequências típicas da turbulência é a difusão, ou seja, o aumento em sistemas abertos da separação entre corpos particulados, em taxas muito superiores àquelas da difusão molecular térmica padrão. Neste trabalho, apresentamos um estudo focado na quantificação da difusão turbulenta de partículas através de simulações numéricas de turbulência, com o objetivo de identificar impactos de fertilização e dispersão de poluentes atmosféricos com implicações na saúde e ambiente / In the present study, we study the diffusion dispersed atmospherically compounds, such as fertilizers and particular pesticides in large scale agricultural environments. This study focuses on the applicability of numerical and theoretical and phenomenological models of turbulent phenomena in estimates of economic and environmental advantages of these systems. The Earth\'s atmosphere, in typical size and speed ranges of the study object of this work is a turbulent system. Turbulence is a complex phenomenon which involves the dynamic interaction of different ranges resulting in a large-scale collective effect due to a nonlinear interaction between perturbation modes in a fluid. The modeling of turbulence, so it is generally possible through Direct Numerical Simulation - DNS. A typical consequence of turbulence is the diffusion, i.e., increased separation in unbound systems of particulate bodies, much higher than those of the standard thermal molecular diffusion rates. In this work we present a study focused on quantifying the turbulent diffusion of particles through numerical simulations of turbulent media, in order to identify the impact of fertilization and dispersion of air pollutants on human health and environment

abstract: Fluctuations with a power spectral density depending on frequency as $1/f^\alpha$ ($0<\alpha<2$) are found in a wide class of systems. The number of systems exhibiting $1/f$ noise means it has far-reaching practical implications; it also suggests a possibly universal explanation, or at least a set of shared properties. Given this diversity, there are numerous models of $1/f$ noise. In this dissertation, I summarize my research into models based on linking the characteristic times of fluctuations of a quantity to its multiplicity of states. With this condition satisfied, I show that a quantity will undergo $1/f$ fluctuations and exhibit associated properties, such as slow dynamics, divergence of time scales, and ergodicity breaking. I propose that multiplicity-dependent characteristic times come about when a system shares a constant, maximized amount of entropy with a finite bath. This may be the case when systems are imperfectly coupled to their thermal environment and the exchange of conserved quantities is mediated through their local environment. To demonstrate the effects of multiplicity-dependent characteristic times, I present numerical simulations of two models. The first consists of non-interacting spins in $0$-field coupled to an explicit finite bath. This model has the advantage of being degenerate, so that its multiplicity alone determines the dynamics. Fluctuations of the alignment of this model will be compared to voltage fluctuations across a mesoscopic metal-insulator-metal junction. The second model consists of classical, interacting Heisenberg spins with a dynamic constraint that slows fluctuations according to the multiplicity of the system's alignment. Fluctuations in one component of the alignment will be compared to the flux noise in superconducting quantum interference devices (SQUIDs). Finally, I will compare both of these models to each other and some of the most popular models of $1/f$ noise, including those based on a superposition of exponential relaxation processes and those based on power law renewal processes. / Dissertation/Thesis / Doctoral Dissertation Physics 2018

Composite materials reinforced with particles or fibers are widely used in industrial applications due to their good mechanical, thermal, and electrical properties. Consequently, for the scientific community as well as the industry, an important challenge is to understand the relationship between the microstruture and the macroscopic response in order to design composite materials with optimised properties. In this thesis, we study a class of inclusion-reinforced multi-phase composites. Our main objective is to develop a micromechanical model and the corresponding numerical algorithms which enable the simulation of the rate-independent mechanical response. The proposed model is based on an incremental Hill-type formulation and uses the two-step Mori-Tanaka/Voigt mean-field homogenisation schemes. The crucial issues of the choice of reference comparison materials and Eshelby's tensor computation are examined In parallel, an experimental study consisting in four-point bending tests performed on plain concrete and steel fiber-reinforced concrete (SFRC) specimens, is carried out with the aim of achieving an appropriate modelling of SFRC, and collecting data for the validation of our model predictions. The accuracy and the efficiency of the proposed approach are evaluated through numerical simulations. Several discriminating tests of concrete, metal, and polymer matrix composites are carried out. A two-scale approach is developed in order to simulate, within reasonable CPU time and memory usage, the response of realistic structures under complex loadings. In many cases our estimates are validated against finite element computations and experimental results.

Numerical simulations of Mach shock reflections have shown that the Mach stem can bifurcate as a result of the slip line jetting forward. Numerical simulations were conducted in this study which determined that these bifurcations occur when the Mach number is high, the ramp angle is high, and specific heat ratio is low. It was clarified that the bifurcation is a result of a sufficiently large velocity difference across the slip line which drives the jet. This bifurcation phenomenon has also been observed after triple point collisions in detonation simulations. A triple point reflection was modelled as an inert shock reflecting off a wedge, and the accuracy of the model at early times after reflection indicates that bifurcations in detonations are a result of the shock reflection process. Further investigations revealed that bifurcations likely contribute to the irregular structure observed in certain detonations.