Previous studies have shown that thermal feedback from protostars plays a key role in the process of low-mass star formation. In this thesis, we explore the effects of protostellar heating on the formation of stellar clusters. We describe new methods for modelling protostellar accretion luminosities and protostellar evolution in calculations of star formation. We then present results of a series of numerical simulations of stellar cluster formation which include these effects, and examine their impact. We begin by investigating the dependence of stellar properties on the initial density of molecular clouds. We find that the dependence of the median stellar mass on the initial density of the cloud is weaker than the dependence of the thermal Jeans mass when radiative effects are included. We suggest that including protostellar accretion luminosities and protostellar evolution may weaken this dependence further, and may account for the observed invariance of the median stellar mass in Galactic star-forming regions. Next, we investigate the effects of including accretion feedback from sink particles on the formation of small stellar groups. We find that including accretion feedback in calculations suppresses fragmentation even further than calculations that only include radiative transfer within the gas. Including feedback also produces a higher median stellar mass, which is insensitive to the sink particle accretion radius used. Finally, we compare calculations of small stellar clusters which model the evolution of protostars using a live stellar model with those which use a fixed stellar structure. We find that the dynamics of the clusters are primarily determined by the accretion luminosities of protostars, but that the relative effects of protostellar evolution depend on the accretion rate and advection of energy into the protostar. We also demonstrate how such calculations may be used to study the properties of young stellar populations.

The radiative transfer equation (RTE) models the transport of radiation through a participating medium. In particular, it captures how radiation is scattered, emitted, and absorbed as it interacts with the medium. This process arises in numerous application areas, including: neutron transport in nuclear reactors, radiation therapy in cancer treatment planning, and the investigation of forming galaxies in astrophysics. As a result, there is great interest in the solution of the RTE in many different fields. We consider the energy dependent form of the RTE and allow media containing regions of negligible absorption. This particular case is not often considered due to the additional dimension and stability issues which arise by allowing vanishing absorption. In this thesis, we establish the existence and uniqueness of the underlying boundary value problem. We then proceed to develop a stable numerical algorithm for solving the RTE. Alongside the construction of the method, we derive corresponding error estimates. To show the validity of the algorithm in practice, we apply the algorithm to four different example problems. We also use these examples to validate our theoretical results.

La génération actuelle des sondeurs infrarouges avancés constitue l’une des sources les plus importantes d’observation dans les systèmes d’assimilation de données dans les modèles de la Prévision Numérique du Temps (PNT). Cependant la richesse d’informations fournies par ce type de capteur avec son grand nombre de canaux et sa couverture globale est loin d’être complètement exploitée. La présence de nuages dans le champ de vision de l’instrument, qui affecte la majorité des observations, est l’une des raisons pour lesquelles les centres de PNT rejettent une grande quantité des observations des sondeurs. Les centres de PNT ont cependant commencé à assimiler au-dessus des océans les radiances affectées par les nuages en utilisant des canaux dont les effets radiatifs nuageux sont modélisés par un modèle de nuage simple. Certains de ces algorithmes de détection sont évalués dans ce manuscrit, et leurs limitations sont explicitées. Afin d’accroître la quantité de données assimilées, il est nécessaire de mieux représenter les nuages et leurs effets radiatifs. Depuis quelques années, des études ont été menées pour mieux représenter leurs effets dans les modèles de transfert radiatif ([Faijan et al., 2012] ; [Martinet et al., 2013]) ; et utiliser dans l’assimilation de nouveaux canaux infrarouges informatifs sur les hydrométéores nuageux. ([Martinet et al., 2014]). Cette thèse se concentre principalement sur ces méthodes de détection de scènes homogènes en consacrant sa majeur partie à l’établissement, l’évaluation et l’amélioration d’algorithme de détection de scènes homogènes en se basant sur la colocalistion d’observation avec d’autres sondeurs. Ces études sont rendus possibles par la prise en compte des champs d’hydrométéores fournis par les schémas convectifs du modèle ARPEGE en entrée du modèle de transfert radiatif nuageux RTTOV-CLD. Une partie validation des simulations est opérée dans cette thèse, en comparant l’apport les forces et faiblesses du schéma convectif en opérationnel ainsi que PCMT. Par la suite, différents tests, ou critères, de détection sont proposés, et en réalisant des expériences d’assimilation et en évaluant l’impact de ces ces critères de sélection proposés sur la qualité des prévisions à longues échéances, un des tests parmi ceux proposés se démarque des autres en conservant une quantité importante d’observation ciel clair et démontre des impacts neutres à légèrement positifs sur les prévisions. Les nouvelles méthodes de sélection de scènes homogènes proposées dans cette études permettent d’envisager une amélioration significative du contrôle de qualité des observation IASI en ciel clair. Cela ouvre ainsi donc la voie à une utilisation, plus maîtrisée, des scènes nuageuses. Nous expliquons dans ce manuscrit pourquoi il serait imprudent de précéder à des assimilation de radiances infrarouge contaminées par la présence de nuages. Pour contourner cette difficulté, une technique d’assimilation en deux étapes déjà utilisé pour l’assimilation des réflectivité radar ([Wattrelot et al., 2014]) dans AROME est évaluée. Cette méthode basée sur l’inversion bayésienne a récemment été adaptée pour les observations microondes satellitaire ([Duruisseau et al., 2018]). Dans cette étude, nous explorons cette technique pour les observations IASI. Plusieurs tests de sensibilité sont effectués sur les différents paramètres de l’algorithme, avec pour objectif de préparer de futurs travaux sur l’assimilation all-sky infrarouges, explicités dans les perspectives de ce manuscrit. / The current generation of advanced infrared sounders is one of the most important sources of observations in data assimilation systems in numerical weather prediction (NWP) models. However, the total amount of information provided by this type of sensor, with its large number of channels and its global coverage, is far from being fully exploited. The presence of clouds in the instrument’s field of view, which affects the majority of observations, is one of the reasons why NWP centers reject a large amount of observations from sounders. NWP centers, however, have begun to assimilate cloud-affected radiances over the oceans using channels whose cloudy radiative effects are modeled by a simple cloud model. Some of these detection algorithms are evaluated in this manuscript, and their limitations are clarified. In order to increase the amount of assimilated data, it is necessary to better represent clouds and their radiative effects in the models. For several years, studies have been conducted to better represent their effects in radiative transfer models ([Faijan et al., 2012] ; [Martinet et al., 2013]) ; and to use new informative infrared channels of cloudy hydrometeors in the assimilation. [Martinet et al., 2014]. This thesis focuses on several approaches for the assimilation of cloudy radiances. In the first part, the characterization of the cloud parameters currently used for the assimilation of cloudy radiances was evaluated in the global and regional scale models. In addition, as part of the "all-sky" assimilation, which considers both clear and cloudy radiances, the evaluation and improvement of homogeneous scene detection algorithms based on the colocation of observations with other imagers was studied. These studies are made possible by taking into account the hydrometeorological fields provided by the convective schemes of the ARPEGE model as the input of the RTTOV-CLD cloud radiative transfer model. Part of this thesis concerns the validation of simulations, by comparing the contribution of the new convective PCMT scheme to the one used in operational applications. Subsequently, different criteria for selecting homogeneous scenes are proposed. By conducting assimilation experiments and evaluating the impact of these proposed selection criteria on the quality of long-term forecasts, one of the proposed tests stands out from the others by keeping a significant amount of clear sky observations and demonstrating neutral to slightly positive impacts on the forecasts. These new methods for selecting homogeneous scenes proposed in this study allows the consideration of improving the quality control of IASI observations in clear sky. To address the issue of all-sky radiance data assimilation, the two-step assimilation technique, already used for radar reflectivity assimilation in AROME ([Wattrelot et al., 2014]), was evaluated for IASI radiances in the ARPEGE model in a case study. This method based on Bayesian inversion has recently been adapted for satellite microwave observations ([Duruisseau et al., 2018]). Several sensitivity tests were carried out on the different parameters of the algorithm, with the objective of preparing for future work on infrared all-sky assimilation, as explained in the perspectives of this manuscript.

Terahertz (THz) spectroscopy can potentially be used to probe and characterize inhomogeneous materials, however spectroscopic identification of such materials from spectral features of diffuse returns is a relatively underdeveloped area of study. In this thesis, diffuse THz scattering from granular media is modeled by applying radiative transfer (RT) theory for the first time in THz sensing. Both classical RT theory and dense media radiative transfer (DMRT) theory based on the quasi-crystalline approximation (QCA) are used to calculate diffuse scattered intensity. The numerical solutions of the vector radiative transfer equations (VRTE) were coded and calculated in MATLAB. The diffuse scattered field from compressed Polyethylene (PE) pellets containing steel spheres was measured in both transmission and reflection using a THz time domain spectroscopy (THz-TDS) system. Measurement results showed energy redistribution by granular media due to volume scattering as well as angle dependent spectral features due to Mie scattering. The RT model was validated by successfully reproducing qualitative features observed in experimental results. Diffuse intensity from granular media containing Teflon, lactose sugar, and C4 explosive was then calculated using the RT models. Simulation results showed the amplitude of diffuse intensity is affected by factors such as grain size, fractional volume of grains, thickness of scattering layer, and scattering angles. Spectral features were also observed in the diffuse intensity spectra from media containing grains with THz spectral signatures. The simulation results suggest the possibility of identifying materials from diffuse intensity spectra.

The atmospheric radiative transfer model MOCARAT was developed and is presented in this thesis. MOCARAT employs a Monte Carlo Technique for the accurate modeling of band radiances and reflectances in an atmospheric system with a ruffled ocean surface as a lower boundary. The atmospheric radiative transfer is modeled with consideration of molecular Rayleigh scattering, Mie Scattering and absorption on particulate matter, as well as band absorption by molecules in the wavelength channels of interest. The bidirectional reflection of downwelling light at the ocean surface is computed using the empirical relationship between surface wind field and the slope distribution of wave facets derived by Cox and Munk (1954a). A method is proposed to use the oceanic sun glint for remote sensing applications. The sensitivity of channel correlations to aerosol burden and type as well as other atmospheric and observational parameters is assessed. Comparisons of observed correlations with model results are used to check the consistency of the calibration of the airborne Multichannel Cloud Radiometer (MCR) that was employed during the Indian Ocean Experiment (INDOEX). The MCR calibration exhibited large variability from flight to flight. The method was applied to MODIS observations. Unlike the MCR, MODIS was stable where expected, although numerical values for some of the wavelengths appear to depart from theory. / Graduation date: 2004

Satellite technology represents the only technique for measuring sea surface temperatures (SSTs) on a global scale. SSTs are important as boundary conditions for climate and atmospheric boundary layer models which attempt to describe phenomena of all scales, ranging from local forecasts to predictions of global warming. Historical use of infrared satellite measurements for SST determination has been based on a theory which assumes that the atmosphere is 'thin', i.e., that atmospheric absorption of infrared radiation emitted from the sea surface has very little effect on the radiant intensity that is measured by satellites. However, a variety of independent radiative transfer models point to the possibility that the so-called 'thin approximation' is violated for humid atmospheres such as those found in the tropics, leading to errors in the retrieved SST that would be unacceptable to those who make use of such products. Furthermore, such tropical regions represent a significant portion of the globe, where coupled ocean-atmosphere disturbances can have global effects (e.g., the tropical Pacific El Nino-Southern Oscillation events). This study evaluates the thin approximation empirically, by combining radiative transfer theory and satellite data from the Eastern Atlantic ocean region studied during the Atlantic Statocumulus Transition Experiment (ASTEX). Six months of satellite data from May, June, and July of 1983 and 1984 are analyzed. To the degree that the data may be considered representative of globally valid relationships between measured variables, it is shown that the thin approximation is not appropriate for the tropics. This suggests that new methods are necessary for retrieving SSTs from the more humid regions of the globe. / Graduation date: 1993

For over 30 years, the Implicit Monte Carlo (IMC) method has been used to solve challenging problems in thermal radiative transfer. These problems are typically optically thick and di ffusive, as a consequence of the high degree of "pseudo-scattering" introduced to model the absorption and reemission of photons from a tightly-coupled, radiating material. IMC has several well-known features which could be improved: a) it can be prohibitively computationally expensive, b) it introduces statistical noise into the material and radiation temperatures, which may be problematic in multiphysics simulations, and c) under certain conditions, solutions can be unphysical and numerically unstable, in that they violate a maximum principle - IMC calculated temperatures can be greater than the maximum temperature used to drive the problem. We have developed a variant of IMC called "iterative thermal emission" IMC, which is designed to be more stable than IMC and have a reduced parameter space in which the maximum principle is violated. ITE IMC is a more implicit method version of the IMC in that it uses the information obtained from a series of IMC photon histories to improve the estimate for the end of time-step material temperature during a time step. A better estimate of the end of time-step material temperature allows for a more implicit estimate of other temperature dependent quantities: opacity, heat capacity, Fleck Factor (probability that a photon absorbed during a time step is not reemitted) and the Planckian emission source. The ITE IMC method is developed by using Taylor series expansions in material temperature in a similar manner as the IMC method. It can be implemented in a Monte Carlo computer code by running photon histories for several sub-steps in a given time-step and combining the resulting data in a thoughtful way. The ITE IMC method is then validated against 0-D and 1-D analytic solutions and compared with traditional IMC. We perform an in finite medium stability analysis of ITE IMC and show that it is slightly more numerically stable than traditional IMC. We find that significantly larger time-steps can be used with ITE IMC without violating the maximum principle, especially in problems with non-linear material properties. We also compare ITE IMC to IMC on a two-dimensional, orthogonal mesh, x-y geometry problem called the "crooked pipe" and show that our new method reproduces the IMC solution. The ITE IMC method yields results with larger variances; however, the accuracy of the solution is improved in comparison with IMC, for a given choice of spatial and temporal grid. / Graduation date: 2013

A two-dimensional model for predicting the rate of radiation heat transfer for the interior of an industrial furnace is described. The model is two-dimensional due to the assumptions of the heat source as an infinite radiating plane and the heat sink as rows of parallel tubes that are both infinite in length and in number. A refractory back wall, located behind the tube rows, is also included in some of the model configurations. The optical properties for the heat source, heat sink, and refractory back wall are simplified by assuming the "black-body" case: all are treated as perfect absorbers and emitters of radiation. This assumption allows three different solution techniques-a graphical, crossed-string, and numerical method-to be used in solving for the radiant transfer rate. The numerical method, an innovative Monte Carlo technique, is the one employed in this study. Hottel used a graphical technique to solve the furnace model for a two row configuration in which the tubes are arranged on equilateral triangular centers. His results, along with those produced by the crossed-string method, are used in this work to validate the numerical technique. Having been validated, the numerical method was then employed to extend Hottel's work by adding more tube rows to the original equilateral triangular configuration and by generalizing the results to isosceles arrangements. Findings of this investigation are summarized in a table that lists the direct view factors for a ten tube row configuration arranged in an equilateral triangular array. Values from this table can be used to solve the transfer rate problem for twenty different cases by assuming a nonconducting refractory back wall. Results for twelve cases are represented graphically in this document The results are used to demonstrate the importance of a refractory back wall on overall radiation absorption. Examinations of the two row and five row cases for an isosceles triangular array indicate that the tabular values can be applied to any isosceles arrangement if the ratio of row separation distance to tube center-to-center distance is 0.7 or greater. / Graduation date: 1995

Liniengetriebene Winde werden durch Impulsübertrag von Photonen auf ein Plasma bei Absorption oder Streuung in zahlreichen Spektrallinien beschleunigt. Dieser Prozess ist besonders effizient für ultraviolette Strahlung und Plasmatemperaturen zwischen 10^4 K und 10^5 K. Zu den astronomischen Objekten mit liniengetriebenen Winden gehören Sterne der Spektraltypen O, B und A, Wolf-Rayet-Sterne sowie Akkretionsscheiben verschiedenster Größenordnung, von Scheiben um junge Sterne und in kataklysmischen Veränderlichen bis zu Quasarscheiben. Es ist bislang nicht möglich, das vollständige Windproblem numerisch zu lösen, also die Hydrodynamik, den Strahlungstransport und das statistische Gleichgewicht dieser Strömungen gleichzeitig zu behandeln. Die Betonung liegt in dieser Arbeit auf der Windhydrodynamik, mit starken Vereinfachungen in den beiden anderen Gebieten. <br /> Wegen persönlicher Beteiligung betrachte ich drei Themen im Detail. <br /> 1. Windinstabilität durch Dopplerde-shadowing des Gases. Die Instabilität bewirkt, dass Windgas in dichte Schalen komprimiert wird, die von starken Stoßfronten begrenzt sind. Schnelle Wolken entstehen im Raum zwischen den Schalen und stoßen mit diesen zusammen. Dies erzeugt Röntgenflashes, die die beobachtete Röntgenstrahlung heißer Sterne erklären können. <br /> 2. Wind runway durch radiative Wellen. Der runaway zeigt, warum beobachtete liniengetriebene Winde schnelle, kritische Lösungen anstelle von Brisenlösungen (oder shallow solutions) annehmen. Unter bestimmten Bedingungen stabilisiert der Wind sich auf masseüberladenen Lösungen, mit einem breiten, abbremsenden Bereich und Knicken im Geschwindigkeitsfeld. <br /> 3. Magnetische Winde von Akkretionsscheiben um Sterne oder in aktiven Galaxienzentren. Die Linienbeschleunigung wird hier durch die Zentrifugalkraft entlang korotierender poloidaler Magnetfelder und die Lorentzkraft aufgrund von Gradienten im toroidalen Feld unterstützt. Ein Wirbelblatt, das am inneren Scheibenrand beginnt, kann zu stark erhöhten Massenverlustraten führen. / Line driven winds are accelerated by the momentum transfer from photons to a plasma, by absorption and scattering in numerous spectral lines. Line driving is most efficient for ultraviolet radiation, and at plasma temperatures from 10^4 K to 10^5 K. Astronomical objects which show line driven winds include stars of spectral type O, B, and A, Wolf-Rayet stars, and accretion disks over a wide range of scales, from disks in young stellar objects and cataclysmic variables to quasar disks. It is not yet possible to solve the full wind problem numerically, and treat the combined hydrodynamics, radiative transfer, and statistical equilibrium of these flows. The emphasis in the present writing is on wind hydrodynamics, with severe simplifications in the other two areas. <br /> I consider three topics in some detail, for reasons of personal involvement. <br /> 1. Wind instability, as caused by Doppler de-shadowing of gas parcels. The instability causes the wind gas to be compressed into dense shells enclosed by strong shocks. Fast clouds occur in the space between shells, and collide with the latter. This leads to X-ray flashes which may explain the observed X-ray emission from hot stars. <br /> 2. Wind runaway, as caused by a new type of radiative waves. The runaway may explain why observed line driven winds adopt fast, critical solutions instead of shallow (or breeze) solutions. Under certain conditions the wind settles on overloaded solutions, which show a broad deceleration region and kinks in their velocity law. <br /> 3. Magnetized winds, as launched from accretion disks around stars or in active galactic nuclei. Line driving is assisted by centrifugal forces along co-rotating poloidal magnetic field lines, and by Lorentz forces due to toroidal field gradients. A vortex sheet starting at the inner disk rim can lead to highly enhanced mass loss rates.

A condensed multigroup formulation is developed which maintains direct consistency with the continuous energy or fine-group structure, exhibiting the accuracy of the detailed energy spectrum within the coarse-group calculation. Two methods are then developed which seek to invert the condensation process turning the standard one-way condensation (from fine-group to coarse-group) into the first step of a two-way iterative process. The first method is based on the previously published Generalized Energy Condensation, which established a framework for obtaining the fine-group flux by preserving the flux energy spectrum in orthogonal energy expansion functions, but did not maintain a consistent coarse-group formulation. It is demonstrated that with a consistent extension of the GEC, a cross section recondensation scheme can be used to correct for the spectral core environment error. A more practical and efficient new method is also developed, termed the "Subgroup Decomposition (SGD) Method," which eliminates the need for expansion functions altogether, and allows the fine-group flux to be decomposed from a consistent coarse-group flux with minimal additional computation or memory requirements. In addition, a new whole-core BWR benchmark problem is generated based on operating reactor parameters in 2D and 3D, and a set of 1D benchmark problems is developed for a BWR, PWR, and VHTR core.