Dans certains regimes hypersoniques, le rayonnement peut enormement modifier l'ecoulement aerodynamique. Pour de telles applications, il est important d'avoir un modele qui realise un couplage fort entre l'hydrodynamique et le transfert radiatif afin d'avoir un bon comportement de la solution. Cependant, le couplage avec l'equation du transfert radiatif est en general extremement couteux et donc peu raisonnable pour des simulations multidimensionnelles instationnaires. Notre choix est d'utiliser un modele aux moments pour la partie rayonnement, ce qui est bien moins couteux. Celui-ci est base sur une fermeture entropique a la Levermore qui permet de conserver les principales proprietes de la physique. On developpe une version multigroupe de ce modele afin de pouvoir traiter des cas realistes tres dependants de la frequence. Le systeme couple resultant est hyperbolique et possede des proprietes interessantes qui sont etudiees. Ce modele radiatif est couple avec les equations de Navier-Stokes avec une approche totalement implicite et fortement couplee. De plus, pour gagner de la place memoire, on choisit d'utiliser une methode sans Jacobienne, en pratique une methode de type GMRes preconditionne. Cette methode se revele assez rapide pour pouvoir simuler des applications realistes a un cout de calcul raisonnable, ce qui n'est pas le cas de la plupart des modeles courament utilises dans la litterature. Plusieurs applications sont donnees pour illustrer le bon comportement du modele a la fois dans des configurations academiques simplifiees ou l'on peut faire des comparaisons et dans des configurations realistes comme l'ecoulement lors de l'entree atmospherique de sondes superorbitales.

Ce travail estime le potentiel des plasmas de striction magnétique (Z-pinches) pour le chauffage de cavités radiatives à haute température (>200eV). Des modèles simples sont fournis pour calculer les performances atteignables avec des courants de 5 à 100 MA en 100 ns. La physique monodimensionnelle à l'échelle de l'épaisseur du plasma et les instabilités hydrodynamiques sont étudiées. Puis l'amélioration des performances des cavités avec une double coquille ou l'installation d'un champ magnétique axial est analysée. L'attaque directe par un Z-pinch d'une cible de fusion par confinement inertiel est enfin considérée. Tous les résultats présentés reposent sur une approche théorique et numérique (bidimensionnelle) et sur l'exploitation de résultats expérimentaux obtenus sur le générateur américain "Z". Les annexes rappellent les équations de la MHD radiative et vérifient leur validité pour les plasmas de striction magnétique.

<p>A major fraction of stars will pass through a short period of dramatic events in their final evolutionary stage. Low- to intermediate-mass stars, studied here, are stripped of their outer parts in a slow massive wind. This mass loss reshapes both the star and the surrounding medium. The formation of the wind is a consequence of the non-linear interaction of a number of physical processes. Stellar pulsations and efficient dust formation are examples of such key processes. Time-dependent theoretical models, in combination with observations, are useful tools for understanding these winds.</p><p>The main object of this thesis has been the physical improvement of a theoretical wind model. Here the coupling between the dust and gas in the wind is studied in further detail, allowing drift. The methods that have been developed earlier to describe the micro-physical interaction are overviewed and summarized. Previously dust has often been assumed to move at the same velocity as gas. New time-dependent wind models are presented where grain drift has been treated self-consistently. Specifically, the coupling between dust and gas in the wind has been modeled more realistically, with descriptions of both the modified momentum and energy balances, and drift dependent dust formation. The results of these new ``drift models'' have been compared with the results of non-drift models. </p><p>A general result of the study is that the effects of drift are significant and difficult to predict if a simple analytical theory is used. It has been found that dust in drift models tends to accumulate in certain dense regions, an accumulation that was not possible without drift. Moreover the new models show an increased variability in the wind structure. The use of drift in dust formation tends to markedly increase the produced dust. Some sets of model parameters lead to a wind without including drift, but a corresponding wind does not form when drift is included -- and vice versa. The effects of drift are important and can probably not be ignored in realistic models.</p>

A major fraction of stars will pass through a short period of dramatic events in their final evolutionary stage. Low- to intermediate-mass stars, studied here, are stripped of their outer parts in a slow massive wind. This mass loss reshapes both the star and the surrounding medium. The formation of the wind is a consequence of the non-linear interaction of a number of physical processes. Stellar pulsations and efficient dust formation are examples of such key processes. Time-dependent theoretical models, in combination with observations, are useful tools for understanding these winds. The main object of this thesis has been the physical improvement of a theoretical wind model. Here the coupling between the dust and gas in the wind is studied in further detail, allowing drift. The methods that have been developed earlier to describe the micro-physical interaction are overviewed and summarized. Previously dust has often been assumed to move at the same velocity as gas. New time-dependent wind models are presented where grain drift has been treated self-consistently. Specifically, the coupling between dust and gas in the wind has been modeled more realistically, with descriptions of both the modified momentum and energy balances, and drift dependent dust formation. The results of these new ``drift models'' have been compared with the results of non-drift models. A general result of the study is that the effects of drift are significant and difficult to predict if a simple analytical theory is used. It has been found that dust in drift models tends to accumulate in certain dense regions, an accumulation that was not possible without drift. Moreover the new models show an increased variability in the wind structure. The use of drift in dust formation tends to markedly increase the produced dust. Some sets of model parameters lead to a wind without including drift, but a corresponding wind does not form when drift is included -- and vice versa. The effects of drift are important and can probably not be ignored in realistic models.

This thesis is based on measurements of aerosol optical and microphysical properties made at inland, coastal and island locations in India. Aerosol vertical distribution measurements have also been made both using surface based and aircraft borne instruments. In addition to these, satellite based measurements (MODIS and OMI) have also been used to estimate regional aerosol radiative forcing over the oceanic regions around India. The measurements at an inland, continental, urban location reveals the large effect of anthropogenic activities on aerosol characteristics at surface and the atmospheric vertical column. A clear seasonality is observed in aerosol optical and microphysical properties as a consequence of modulation by anthropogenic activities and the effect of meteorological parameters like rainfall, winds and boundary layer dynamics. The variability observed at different time scales (from diurnal, weekly, monthly to annual) reveals the importance of anthropogenic and natural processes in modulating the aerosol loading. The estimates of aerosol radiative forcing at surface were as high as ~ 40W m-2. A large discrepancy was observed between the observed and modeled aerosol forcing efficiency (forcing per unit optical depth) at surface. These discrepancies are due to the inadequate representation of aerosol mixing state in models. In addition, the large difference found in the observed forcing between winter and summer could also be influenced due to the presence of elevated aerosols during the summer. Measurements made over coastal and central India shows that a large fraction (75-85%) of aerosol column optical depth was contributed by aerosols located above 1 km. The horizontal gradients were sharp with e-1 scaling distance as small as ~250 km in the well-mixed regions mostly under the influence of local source effects. However, above the atmospheric boundary layer, the gradients were much shallower (~800 to 1200 km). In addition, a large fraction (60-75%) of aerosol was found located above clouds leading to enhanced aerosol absorption. Large spatial gradient in aerosol optical depth and hence radiative impacts between the coastal landmass and the adjacent oceans within a short distance of <300 km (even at an altitude of 3 km) during summer and pre-monsoon is of importance to regional climate. Observations at Minicoy, a remote island in southern Arabian Sea to study the characteristics of transported aerosols reveals variability at daily, weekly, monthly and seasonal time scales associated with changes in precipitation and air mass characteristics. The daily mean Black Carbon (BC) mass mixing ratio varied between as low as ~ 0.2 to 9.0%. The resultant average aerosol atmospheric forcing for the observation period was ~15 W m-2. Trajectory based cluster analysis has shown six distinct advection/transport pathways influencing aerosol characteristics over southern Arabian Sea. The Indo-Gangetic Plain, northern Arabian Sea and west Asia are identified to be the most important source regions having a major impact on aerosols loading over the southern Arabian Sea. The cluster analysis, concentration weighted trajectory (CWT) analysis and the MODIS retrievals show an asymmetry in aerosol characteristics between the Arabian Sea and the Bay of Bengal, with the Arabian Sea characterized by large loading by natural aerosols (eg., dust and sea salt) and the Bay of Bengal characterized by anthropogenic loading (eg., BC). The low value of the BC mass mixing ratio measured at the island (mostly ~ 1 to 1.6%), has major implications for regional radiative forcing. The annually averaged net aerosol atmospheric forcing was as low as ~1.7 W m-2 with highest forcing corresponding to IGP cluster. The single scattering albedo (SSA) which is an important parameter in the estimation of aerosol radiative forcing was retrieved by utilizing a joint OMI-MODIS retrieval methodology. The SSA over the oceanic regions around India shows that the largest absorption (SSA < 0.9) occurs during winter. The largest gradients in AOD and SSA were observed over Arabian Sea during the summer as a result of large dust emissions. The largest forcing observed also was confined to the northern Arabian Sea (~ 37 W m-2) as a result of high aerosol column loading and dust transport. The observed annual mean forcing at Minicoy were comparable to that estimated using satellite measurements, but were much lower than those observed during INDOEX.

L'objectif de ce document est de présenter une étude sur la réaction de capture neutronique radiative du noyau instable du ¹⁷³Lu afin de déterminer sa section efficace (n,γ). Si globalement, pour les noyaux stables de nombreuses informations sont à disposition, il reste un véritable manque de données pour les noyaux radioactifs. La première partie de cette thèse se consacre à la présentation des différents formalismes impliqués dans le calcul d'une section efficace ainsi qu'à l'utilisation du code TALYS basé sur ces différents modèles. TALYS nous a permis d'évaluer la section efficace (n,γ) sur le ¹⁷³Lu en s'appuyant sur la connaissance de la réaction de capture sur le ¹⁷⁵Lu. Dans un deuxième temps, la section efficace (n,γ) sur le ¹⁷³Lu a été mesurée sur l'installation LANSCE avec le détecteur 4π DANCE. Cette expérience s'est révélée être un véritable défi tant pour la fabrication de la cible de ¹⁷³Lu que pour l'obtention de données dû à la grande radioactivité de cet isotope. Nous avons pu extraire des informations intéressantes comme le taux de capture total, identifier et caractériser de nouvelles résonances, déterminer des paramètres comme l'espacement moyen, les largeurs neutroniques et les largeurs γ ainsi que la valeur de la fonction densité. Tous ces nouveaux renseignements nous ont permis de reconstruire la section efficace (n,γ) sur le ¹⁷³Lu jusqu'à 200 eV. Grâce à ces différentes informations, nous avons estimé une correction à appliquer sur la section efficace évaluée par TALYS permettant in fine d'obtenir une nouvelle évaluation de cette quantité. La troisième partie de cette thèse est consacrée à apporter des informations supplémentaires sur la réaction ¹⁷³Lu(n,γ)¹⁷⁴Lu en utilisant la méthode de substitution. En premier lieu, nous avons testé la validité de cette méthode sur une réaction connue : ¹⁷⁵Lu(n,γ)¹⁷⁶Lu avec la réaction ¹⁷⁴Yb(³He,p)¹⁷⁶Lu puis dans un second temps nous avons regardé la réaction ¹⁷³Lu(n,γ)¹⁷⁴Lu avec la réaction ¹⁷⁴Yb(³He,t)¹⁷⁴Lu. Pour cela, la probabilité d'émission γ dans ces deux voies a été mesurée et comparée à un calcul TALYS. Cette comparaison a révélé de grandes disparités entre les réactions de transfert utilisées et les réactions induites par des neutrons. Notre investigation s'est alors orientée à regarder de plus près la distribution de spins du noyau composé formé. Celle-ci a pu être extraite grâce à un ajustement de la probabilité d'émission γ mesurée. Cette distribution montre que les réaction (³He,X) peuplent en réalité des spins beaucoup plus grands que ceux issus de la réaction (n,γ). La mesure des rapports des intensités de transitions γ corroborent aussi ce résultat même si les spins peuplés semblent être plus faibles. Cette expérience a mis clairement en évidence qu'une réaction induite par un faisceau d'³He ne pouvait pas se substituer à une réaction (n,γ). Tout au long de ce document, nous avons montré par différents aspects, à quel point il peut être difficile d'obtenir des informations sur les noyaux radioactifs tels que le ¹⁷³Lu et que pour le futur de nombreux défis tant expérimentaux que théoriques sont encore à relever.

The role of scalar mesons in radiative vector meson decays is investigated. The effects of scalar-isoscalar f_{0}(980) and scalar-isovector a_{0}(980) mesons are studied in the mechanism of the radiative Phi-&gt / pi{+}pi{-}gamma and phi-&gt / pi{0}eta gamma decays, respectively. A phenomenological approach is used to study the radiative phi-&gt / pi{+}p{-}gamma decay by considering the contributions of sigma-meson, rho-meson and f_{0}-meson. The interference effects between different contributions are analyzed and the branching ratio for this decay is calculated. The radiative phi-&gt / pi{0}eta gamma decay is studied within the framework of a phenomenological approach in which the contributions of rho-meson, chiral loop and a_{0}-meson are considered. The interference effects between different contributions are examined and the coupling constants g_{phi a_{0} gamma} and g_{a_{0}K{+}K{-}} are estimated using the experimental branching ratio for the phi-&gt / pi{0}eta gamma decay. Furthermore, the radiative rho{0}pi{+}pi{-}gamma$ and rho{0}-&gt / pi{0}pi{0}gamma decays are studied to investigate the role of scalar-isoscalar sigma-meson. The branching ratios of the rho{0}-&gt / pi{+}pi{-}gamma and rho{0}-&gt / pi{0}pi{0}gamma decays are calculated using a phenomenological approach by adding to the amplitude calculated within the framework of chiral perturbation theory and vector meson dominance the amplitude of sigma-meson intermediate state. In all the decays studied the scalar meson intermediate states make important contributions to the overall amplitude.

Nuclear reactor design requires the calculation of integral core parameters and power and radiation profiles. These physical parameters are obtained by the solution of the linear neutron transport equation over the geometry of the reactor. In order to represent the fine structure of the nuclear core a very small geometrical mesh size should be used, but the computational capacity available these days is still not enough to solve these transport problems in the time range (hours-days) that would make the method useful as a design tool. This problem is traditionally solved by the solution of simple, smaller problems in specific parts of the core and then use a procedure known as homogenization to create average material properties and solve the full problem with a wider mesh size. The iterative multi-level solution procedure is inspired in this multi-stage approach, solving the problem at fuel-pin (cell) level, fuel assembly and nodal levels. The nested geometrical structure of the finite element representation of a reactor can be used to create a set of restriction/prolongation operators to connect the solution in the different levels. The procedure is to iterate between the levels, solving for the error in the coarse level using as source the restricted residual of the solution in the finer level. This way, the complete problem is only solved in the coarsest level and in the other levels only a pair of restriction/interpolation operations and a relaxation is required. In this work, a multigrid solver is developed for the in-moment equation of the spherical harmonics, finite element formulation of the second order transport equation. This solver is implemented as a subroutine in the code EVENT. Numerical tests are provided as a standalone diffusion solver and as part of a block Jacobi transport solver.

The role of $f_{0}(980)$ and $a_{0}(980)$ scalar meson intermediate states in the mechanism of radiative $phi (1020)$ meson decay into two charged $K (494)$ mesons and a photon $phirightarrow K^{+} + K^{-} + gamma$ is investigated. For the contribution of scalar meson intermediate state two models are considered. In the kaon-loop model, the scalar meson intermediate state couples the final state to the initial $phi$ meson through a charged kaon-loop. The second model, called no-structure model, consist of point-like coupling of intermediate scalar meson state to the initial state. It is found that in the kaon-loop model, scalar meson intermediate state results in a considerable modification of the pure Bremsstrahlung photon spectrum.

Climate models are the primary tools used for understanding past climate variations and for future projections. The atmospheric radiation is the key component of these models. Accurate modeling of atmosphere necessitates reliable evaluation of the medium radiative properties and accurate solution of the radiative transfer equation in conjunction with the time-dependent multi-dimensional governing equations of atmospheric models. Due to difficulty in solving the equations of atmospheric and radiation models simultaneously, radiation equations have been solved when input data such as concentration, temperature etc. were made available upon solution of equations of atmospheric models. Generally, time step of conservation equations are 10-30 minutes but radiative transfer equation is called only once every 1-3 hours. However, there is inaccuracy due to the fixed radiation fluxes over the intervening time steps. To overcome this problem, the equations of atmospheric and radiation models have to be solved simultaneously and the solution methods have to be compatible. For this purpose, a radiative-convective model with radiation model based on method of lines (MOL) solution of discrete ordinate method (DOM) with wide band correlated-k (WBCK) was developed. To achieve this objective, a previously developed MOL solution of DOM with WBCK model was adapted to 1-D longwave clear sky atmosphere and its predictive accuracy and computational efficiency was examined on the test problem by using benchmark solution obtained from Line-by-line Radiative Transfer Model (LBLRTM). The radiation code was then coupled with radiative-convective model and the predictive accuracy of this model was examined for several coupling intervals. Comparisons reveal that as coupling interval increases, although the computation time of the model decreases, the predicted temperature profiles diverge from the one obtained when equations of radiative-convective model and the radiation model are solved simultaneously and percentage relative error in temperature increases an order of magnitude when coupling time between radiative-convective model and the radiation model increases from 2 to 10 hours. Therefore, it can be concluded that the equations of the radiation model have to be solved simultaneously with the equations of the climate model. Overall evaluation of the performance of the radiation model used in this study points out that it provides accurate and computationally efficient solutions and can be used with confidence in conjunction with the climate models for simultaneous solution of governing equations with radiation transfer equation.