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Cette thèse porte sur la rhéologie des pâtes granulaires. L'image classique pour les pâtes granulaires est qu'il y a une transition d'un écoulement frictionnel vers un écoulement lubrifié lors de l'augmentation du taux de cisaillement. Nous montrons qu'il existe en réalité une transition d'un écoulement localisé vers un écoulement non-localisé. Le paramètre pertinent caractérisant cette transition est le nombre de Leighton, qui est le rapport entre les forces lubrifiée et frictionnelle. Ce nombre définit un taux de cisaillement critique au-dessous duquel aucun écoulement stationnaire sans localisation ne peut exister. Par ailleurs, en menant à la fois des expériences en IRM et des expériences de rhéologie classique, nous définissons une viscosité pour les pâtes granulaires. Il faut pour cela tenir compte de la migration des particules vers les zones faiblement cisaillées lors de l'écoulement, migration qui engendre un profil de concentration des particules. La viscosité est donnée par une loi constitutive constituée de trois équations : l'équation de la courbe d'écoulement, l'équation de Krieger-Dougherty, et le rapport entre contrainte de cisaillement et première différence de contraintes normales. Enfin, nous étudions des suspensions rhéoépaississantes de fécule de maïs qui présentent également une transition d'un régime localisé vers un régime non-localisé autour d'un seuil de rhéoépaississement.

My dissertation, “Africans, Cherokees, and the ABCFM Missionaries in the Nineteenth Century: An Unusual Story of Redemption,” assesses the experience of American missionaries in the Cherokee nation and in Western Africa during the nineteenth century. The American Board of Commissioners for Foreign Missions (ABCFM), founded in 1810, was the first successful foreign missionary society in the U.S., and its campaign among the Cherokees served as springboard for its activities in “Western Africa”—Liberia, Ivory Coast, Gabon, and South Africa. Although the Cherokees and the West Africans were two different peoples, the ABCFM used the same method to Christianize them: the Lancasterian method with which the missionaries planned to “civilize” the Cherokees and West Africans before Christianizing them. Scholars such as William McLoughlin and Theda Purdue studied the missionary perspective and the Cherokee perspective as separate entities and convincingly maintained that the Cherokees embraced the ABCFM’s civilization and Christianization program partly to relieve the pressures on their lands and partly to adapt to the cultural pressures of their times. However, as my dissertation argues, the conversion story of the Cherokees takes a different turn if told simultaneously from the missionary and the Cherokee perspectives. Regarding the West African experience, authors such as Lamin Sanneh and Richard Gray have recently exposed the missionary and African sides of the stories with new questions that had been waiting to be asked for a long time. My dissertation, taking a unique comparative perspective, reveals first that West Africans did not face the same pressures as those faced by the Cherokees, yet, they still embraced the ABCFM’s civilization and Christianization program, though with a lesser sense of urgency and with more assertiveness than did the Cherokees despite the white missionaries’ racism. More importantly, by way of a method I call parallel agency, my dissertation offers a revisionist interpretation of the history of missions, which has traditionally emphasized the power of the white missionaries by calling into question the very assumption that the white missionaries had significantly more power than did their Cherokee and African converts.

Our Sun is a variable star. The magnetic fields in the Sun play an important role for the existence of a wide variety of phenomena on the Sun. Among those, sunspots are the slowly evolving features of the Sun but solar ares and coronal mass ejections are highly dynamic phenomena. Hence, the solar magnetic fields could affect the Earth directly or indirectly through the Sun's open magnetic flux, solar wind, solar are, coronal mass ejections and total solar irradiance variations. These large scale magnetic fields originate due to Magnetohydrodynamic dynamo process inside the solar convection zone converting the kinetic energy of the plasma motions into the magnetic energy. Currently the most promising model to understand the large scale magnetic fields of the Sun is the Flux Transport Dynamo (FTD) model. FTD models are mostly axisymmetric models, though the non-axisymmetric 3D FTD models are started to develop recently. In these models, we assume the total magnetic fields of the Sun consist of poloidal and toroidal components and solve the magnetic induction equation kinematicaly in the sense that velocity fields are invoked motivated from the observations. Differential rotation stretches the poloidal field to generate the toroidal field. When toroidal eld near the bottom of the convection zone become magnetically buoyant, it rises through the solar convection zone and pierce the surface to create bipolar sunspots. While rising through the solar convection zone, the Coriolis force keeps on acting on the flux tube, which introduces a tilt angle between bipolar sunspots. Since the sunspots are the dense region of magnetic fields, they diffuse away after emergence. The leading polarity sunspots (close to equator) from both the hemisphere cancel each other across the equator and trailing polarity sunspots migrate towards the pole to generate effective poloidal fields. This mechanism for generation of poloidal field from the decay of sunspots is known as Babcock-Leighton process. After the poloidal field is generated, the meridional flow carries this field to the pole and further to the bottom of the convection zone where differential rotation again acts on it to generate toroidal field. Hence the solar dynamo goes on by oscillation between the poloidal field and toroidal field, where they can sustain each other through a cyclic feedback process. Just like other physical models, FTD models have various assumptions and approximations to incorporate these different processes. Some of the assumptions are observationally verified and some of them are not. Considering the availability of observed data, many approximations have been made in these models on the theoretical basis. In this thesis, we present various studies leading to better understanding of the different processes and parameters of FTD models, which include magnetic buoyancy, meridional circulation and Babcock-Leighton process. In the introductory Chapter 1, we first present the observational features of the solar magnetic fields, theoretical background of the FTD models and motivation for investigating different processes. Most of the results of our work are presented in Chapters 2 - 7. In the Chapters 2 - 5, we explain various important issues regarding the treatment of magnetic buoyancy, irregularities of the solar cycle during descending phase, effect of different spatial structure of meridional flow on the dynamo and how dynamo generated fields would a ect the meridional ow using 2D axisymmetric Flux Transport Dynamo model. In the Chapters 6 & 7, the build up of polar fields from the decay of sunspots and a proper treatment of Babcock-Leighton process by invoking realistic convective flows, are presented using 3D Flux Transport Dynamo model. Finally the conclusions and future works are given in the Chapter 8. In 2D axisymmetric Flux Transport Dynamo models, the rise of the toroidal magnetic field through the convection zone due to magnetic buoyancy and then the generation of the poloidal magnetic field from these bipolar sunspots, has been treated mainly in two ways|a non-local method and a local method. In Chapter 2, we have analyzed the advantages and disadvantages of both the methods. We find that none of them are satisfactory to depict the correct picture of magnetic buoyancy because it is an inherently 3D process. Unless we go to the 3D framework of Flux Transport Dynamo models, we have to treat the magnetic buoyancy in such simplistic way. We find that the non-local treatment of magnetic buoyancy is very robust for a large span of parameter space but it does not take into account the depletion of flux from the bottom of the convection zone which has a significant importance in irregularity study of the solar cycle. The local treatment of magnetic buoyancy includes the flux depletion from the bottom of the convection zone and treats the magnetic buoyancy much realistically than the non-local treatment. But this local treatment of magnetic buoyancy is not so robust. We also pointed out that the long-standing issue about appearance of sunspots in the low-latitudes needs to be studied carefully. In Chapter 3, we have studied various irregularities of the solar cycle during its decaying phase. We have reported that the decay rate of the cycle is strongly correlated with amplitude of the same cycle as well as the amplitude of the next cycle from different sunspot proxies like sunspot number, sunspot area and 10.7 cm radio flux data. We explain these correlation from flux transport dynamo models. We nd that the correlations can only be reproduced if we introduce stochastic fluctuations in the meridional circulations. We also reproduced most of the correlation found in ascending and descending phase of the solar cycle from century long sunspot area data (Mandal et al., 2017) from Kodaikanal observatory, India which are in great agreement with the correlations found earlier from Greenwich sunspots data. In most of the FTD models, a single cell meridional circulation is assumed within the solar convection zone, with the equatorward return flow at its bottom. But with recent development in helioseismology, plenty of results have come out about various spatial structure of meridional circulation (Zhao et al., 2013; Schad et al., 2013; Rajaguru & Antia, 2015; Jackiewicz et al., 2015). Some helioseismology group (Zhao et al., 2013) reported that the meridional circulation has a double cell structure in solar convection zone and some groups (Schad et al., 2013; Jackiewicz et al., 2015) have reported a multi-cellular structure of meridional circulation in the convection zone. By probing the supergranular motion Hathaway (2012) estimated that the meridional ow has an equatorward return ow at the upper convection zone 70 Mm below the surface. In view of the above observed results, we have discussed in Chapter 4 what would happen to Flux Transport Dynamo model if we consider other structure of meridional circulation instead of single cell meridional circulation encompassing whole convection zone. We nd that the our dynamo model works perfectly ne as long as there is an equatorward propagation at the bottom of the convection zone. Our model also works with shallow meridional circulation as found by Hathaway (2012), if we consider the latitudinal pumping in our model. The temporal variation of meridional circulation on the surface is also observed from various measurement techniques. Chou & Dai (2001) rst observed a variation of meridional circulation with the solar cycle from their helioseismic measurements. Hathaway & Rightmire (2010) also found a variation up to 5 m s 1 for the solar cycle 23 by measuring the magnetic elements on the surface of the Sun. Recently Komm et al. (2015) have analyzed MDI and HMI Dopplergram data and reported a solar cyclic variation with detail latitudinal dependence. To explain this variation of the meridional circulation with the solar cycle, we construct a theoretical model by coupling the equation of the meridional circulation (the component of the vorticity equation within the solar convection zone) with the equations of the flux transport dynamo model in Chapter 5. We consider the back reaction due to the Lorentz force of the dynamo-generated magnetic fields and study the perturbations produced in the meridional circulation due to it. This enables us to model the variations of the meridional circulation without developing a full theory of the meridional circulation itself. We obtain results which reproduce the observational data of solar cycle variations of the meridional circulation reasonably well. We get the best results on assuming the turbulent viscosity acting on the velocity field to be comparable to the magnetic diffusivity (i.e. on assuming the magnetic Prandtl number to be close to unity). We have to assume an appropriate bottom boundary condition to ensure that the Lorentz force cannot drive a flow in the sub-adiabatic layers below the bottom of the tachocline. Our results are sensitive to this bottom boundary condition. We also suggest a hypothesis how the observed inward flow towards the active regions may be produced. In Chapter 6 and Chapter 7, we have studied some of the aspects of solar magnetic eld generation process using 3D dynamo model that were not possible to study earlier using axisymmetric 2D Flux Transport dynamo models. We have used the 3D dynamo model developed by Mark Miesch (Miesch & Dikpati, 2014; Miesch & Teweldebirhan, 2016) and study how polar fields build up from the decay of sunspots more realistically in Chapter 6. We first reproduce the observed butter y diagram and periodic solution considering higher diffusivity value than earlier reported results and use it as a reference model to study the build up polar fields by putting a single sunspot pair in one hemisphere and two sunspot pairs in both the hemispheres. The build up of the polar fields from the decay of sunspots are studied earlier using Surface Flux Transport model (Wang et al., 1989; Baumann et al., 2004; Cameron et al., 2010) which solve only radial component of the induction equation on the surface of the Sun ( | plane). But these 2D SFT models have some inherent limitation for not considering the 3D vectorial nature of the magnetic fields and subsurface processes. We have shown that not considering the vectorial nature and subsurface process has an important effect on the development of the polar fields. We have also studied the effect of a few large sunspot pairs violating Hale's law on the strength of the polar field in this Chapter. We nd that such ant-Hale sunspot pairs do produce some effect on the polar fields, if they appear at higher latitudes during the mid-phase of the solar cycle|but the effect is not dramatic. In Chapter 7, we have incorporated observed surface convective ows directly in our 3D dynamo model. As we know that the observed convective flows on the photosphere (e.g., supergranulation, granulation) play a key role in the Babcock-Leighton (BL) process to generate large scale polar fields from sunspots fields. In most surface flux transport (SFT) and BL dynamo models, the dispersal and migration of surface fields is modeled as an effective turbulent diffusion. Recent SFT models have incorporated explicit, realistic convective flows in order to improve the fidelity of convective transport but, to our knowledge, this has not yet been implemented in previous BL models. Since most Flux-Transport (FT)/BL models are axisymmetric, they do not have the capacity to include such flows. We present the first kinematic 3D FT/BL model to explicitly incorporate realistic convective flows based on solar observations. Though we describe a means to generalize these flows to 3D, we find that the kinematic small-scale dynamo action they produce disrupts the operation of the cyclic dynamo. Cyclic solution is found by limiting the convective flow to surface flux transport. The results obtained are generally in good agreement with the observed surface flux evolution and with non-convective models that have a turbulent diffusivity on the order of 3 1012 cm 2 s 1 (300 km2 s 1). However, we nd that the use of a turbulent diffusivity underestimates the dynamo efficiency, producing weaker mean fields than in the convective models. Also, the convective models exhibit mixed polarity bands in the polar regions that have no counterpart in solar observations. Also, the explicitly computed turbulent electromotive force (emf) bears little resemblance to a diffusive flux. We also find that the poleward migration speed of poloidal flux is determined mainly by the meridional flow and the vertical diffusion.

China has become a major contributor to world science today, with the largest number of qualified scientific publications in the world, a centralized government willing to sponsor the development of science, and pioneering scientists in all disciplines. Where did this scientific power emerge from historically and how did this history connect with the rest of the world? My dissertation suggests that comprehending the Sino-American intellectual exchange network since the early twentieth century is essential for us to grasp the development of science in modern China. It argues that a Sino-American intellectual exchange network through the China Foundation for the Promotion of Education and Culture (ie., the China Foundation) played a critical role in the development of modern scientific research and education from the 1920 to the 1940s. In the first half of the twentieth century, leading American intellectuals of the progressive era such as Teachers College’s educational scholar Paul Monroe and Columbia University’s prominent philosopher of pragmatism John Dewey frequently communicated with prominent Chinese intellectuals, many of whom were their former students in the United States. Such face-to-face interchanges across the Pacific ultimately influenced Chinese choices in shaping modern scientific education and research. The impact was generated primarily through the China Foundation. The China Foundation, financed by the second American remission of the Boxer Indemnity Funds, served as a sponsor of the development of scientific research, teaching and training in modern China. The trustees of the foundation, responsible for the custody and administration of the fund, included prominent Chinese intellectuals (most of whom had received western graduate training) such as Hu Shi (PhD, Columbia), Jiang Menglin (PhD, Teachers College), Zhang Boling (visiting fellow at Teachers College, 1917-1918), Ren Hongjun (H. C. Zen, MA, Columbia), Guo Bingwen (PhD, Teachers College), Ding Wenjiang (aka V. K. Ting, BA, University of Glasgow), Zhao Yuanren (aka Y. R. Chao, PhD, Harvard) as well as the American intellectuals and reformers Paul Monroe, John Dewey, Roger Sherman Greene and John Leighton Stuart. This dissertation researches the history of Sino-American intellectual exchanges in the China Foundation network, which were central to the establishment of science in modern China. It begins by tracing the cohort of leading Chinese intellectuals trained at American universities, who paved the way for its establishment. They invited leading American educators like John Dewey and Paul Monroe to China, and did the translation work that allowed for their reformist ideas of democracy, education and science to become popular in China. While the American intellectuals aspired to transmit a democratic education through introducing science, the Chinese intellectuals also developed their own rationales to pursue China’s scientific modernization. It also examines the political assumptions and tensions wound up in this Sino-American educational exchange network that illuminates the ways in which the intellectuals on both sides of the Pacific were mutually influenced by their intellectual exchanges. In asks the following questions: How did American intellectuals of the progressive era design and pursue a democratic vision for the Chinese scientific development, and what were their political assumptions undergirding the transmission of science? How did the Chinese intellectuals respond to the American knowledge of science, translate, and negotiate this transmission of science to China? What aspects of science did they absorb and incorporate for the Chinese national purposes? What ideas did they absorb from the United States, and what aspects did they deliberately eschew? In posing these questions, part of my goal is to shift the predominant narrative of transnational progressive era US intellectual history from “Atlantic Crossings” to a dense and constitutive set of exchanges of knowledge, ideas and practices of sciences across the Pacific.