Le but de cette étude est de comprendre les relations entre les roches carbonatées et les paléofluides qui les traversent. Les études paléogéographiques et les descriptions géologiques ainsi que les analyses géochimiques des roches réservoirs ont été réalisées sur la Formation de Mishrif dans le champ pétrolier de Nasiriya (sud-est de l’Iraq). Les données de 5 forages carrotés (NS-1 à NS-5), les rapports de prospections et les données de production du champ de Nassiriya, ont été utilisés. Les analyses des microfaciès montrent que la Formation de Mishrif contient une grande variété d’organismes tels que des formaminifères, des coraux, des rudites ainsi que des algues, microbialites, des pellets, des peloides, des grains aggrégé et des grains arrondis. Par conséquent, la formation de Mishrif serait représentative d’un environnement d’eau de subsurface de la zone évaporitique jusqu’à la zone de récif arrière. Le système de transport des fluides dans la Formation de Mishrif se fait au travers des réseaux de stylolite, des fractures ainsi que du réseau poral. Les inclusions des fluides aqueuses sont composées du système H2O-MgCl2. Les températures homogènes des inclusions des fluides aqueuses varient entre 150 et 175 °C. Les températures homogènes des inclusions des fluides pétrolières représentent les degrés élevés de 225 à 250 °C. Les processus de cimentation indiquent quatre phases d’évènements. La première phase a eu lieu avant la migration d’hydrocarbure. La seconde phase s’est produite pendant la migration de ces hydrocarbures. La troisième phase arrive après le processus de migration. Enfin, la quatrième phase est représentée par la distribution du bitume. / The aim of the present study is related to understand the paleofluid-rock interactions in carbonate rocks and its relation with oil potential during upper Cretaceous. Paleogeography studies, geological descriptions and geochemistry analyses of the reservoir rocks were conducted on the Mishrif Formation of the Nasiriah oil field (south-east of Iraq). The data of drill cores from 5 drillholes (NS-1 to NS-5), exploration reports and production data of the Nasiriyah oil field have been used. The microfacies analyses show that Mishrif includes foraminifera, coral, ruddiest, algae, microbialite, favreina microcoprolite, pellets, peloids, aggregate grains and rounded clastic grains. Therefore, shallow-water environments represent Mishrif paleoenvironments, included evaporitic zone to the back-reef zone of the interior carbonate platform shelf. Transport system in the Mishrif contains stylolite networks, fractures and porosity systems. The scanning electron microscope (SEM) shows the balanced distribution of the transport systems regardless of the microfacies type. The aqueous fluid inclusions are mainly composed of H2O-MgCl2 system. Homogeneous temperatures of the aqueous fluid inclusions range from 150 to 175°C. Homogeneous temperatures of the petroleum fluid inclusions in the latter fractures represent high degrees from 225 up to 250°C. Cementation process exhibits four phases of the cementation events. The first phase took place before the hydrocarbon migration. The second occurred during the hydrocarbon migration. Third phase happened after process of the hydrocarbon migration and the last phase represented the thermochemical sulfate reduction by the distribution of bitumen.

No description available.

No description available.

Digitized by Kansas Correctional Industries

1 / Amanda Rosemary Pahng

Thesis--Ohio State University. / Includes bibliographical references. Available online via OhioLINK's ETD Center

Colloidal gas aphrons (CGAs) recently used as part of water-based drilling fluids have been found effective in controlling the filtration rate by bridging the pores of the reservoir rock and therefore, reducing the formation damage. This research aims to generate colloidal gas aphrons (CGA) in oil based drilling fluids; to study stability, rheology and the filtration loss characteristics of CGAs and to investigate formation damage properties of CGAs as a drilling fluid. Aphrons were generated in mineral oil using a polymer-surfactant mix. Based on how changing the polymer and surfactant concentration affects the physico-chemical characteristics of the fluid, an optimum formulation for the aphron drilling fluid was suggested. The stability of microbubbles was investigated by looking at the effects of time, temperature and pressure on the aphron yield and bubble size distribution. Effects of temperature and pressure on the density of the oil-based aphron fluids have been investigated. Based on the PVT analysis results, an equation of state was proposed. Finally, the performance of the oil-based aphron fluid in porous media was investigated. The effects of changing the CGA fluid injection rate, the type of saturating fluid and the wettability of the porous media on the pressure drop were examined. An assessment of the formation damage following the oil-based CGA fluid injection was also made. / Petroleum Engineering

This dissertation presents the configuration and capacity management of manufacturing cells using cluster analysis. A heuristic based on cluster analysis is developed to solve cell formation in cellular manufacturing systems (CMS). The clustering heuristic is applied for cell formation considering processing requirement (CFOPR) as well as various manufacturing factors (CFVMF). The proposed clustering heuristic is developed by employing a new solving structure incorporating hierarchical and non-hierarchical clustering methods. A new similarity measure is constructed by modifying the Jarccard similarity and a new assignment algorithm is proposed by employing the new pairwise exchange method. In CFOPR, the clustering heuristic is modified by adding a feedback step and more exact allocation rules. Grouping efficacy is employed as a measure to evaluate solutions obtained from the heuristic. The clustering heuristic for CFOPR was evaluated on 23 test problems taken from the literature in order to compare with other approaches and produced the best solution in 18 out of 23 and the second best in the remaining problems. These solutions were obtained in a considerably short time and even the largest test problem was solved in around one and a half seconds. In CFVMF, the machine capacity was first ensured, and then manufacturing cells were configured to minimize intercellular movements. In order to ensure the machine capacity, the duplication of machines and the split of operations are allowed and operations are assigned into duplicated machines by the largest-first rule. The clustering heuristic for CFVMF proposes a new similarity measure incorporating processing requirement, material flow and machine workload and a new machine-part matrix representing material flow and processing time assigned to multiple identical machines. Also, setup time, which has not been clearly addressed in existing research, is discussed in the solving procedure. The clustering heuristic for CFVMF employs two evaluation measures such as the number of intercellular movements and grouping efficacy. In two test problems taken from the literature, the heuristic for CFVMF produced the same results, but the trade-off problem between the two evaluation measures is proposed to consider the goodness of grouping.

In this thesis, we focus on obtaining and interpreting observational information on (i) the role of multiplicity on the properties of young stars; (ii) the early evolutionary influence of circumstellar disks; and (iii) the nature of accretion in young systems. To facilitate this research, we conducted an extensive multi-epoch high-resolution spectroscopic survey at optical wavelengths (3,200-10,000 A) of ~200 T Tauri stars in the ~2 Myr old Chamaeleon I, and Taurus-Auriga star-forming regions with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph on the Magellan Clay 6.5 m telescope. From the spectroscopic data, we identify eight close binaries and four close triples, of which three and two, respectively, are new discoveries. We find that the multiplicity fraction for Cha I and Tau-Aur are similar to each other, and to the results of field star surveys. The frequency of systems with close companions in our sample is not seen to depend on primary mass or accretion. We probed for evidence of disk braking. We did not see a statistically significant difference between the distribution of rotational velocities with the presence of an inner disk. Also, our findings show that F-K stars in our sample have larger rotational velocities and specific angular momentum than M stars. We also analyzed accretion variability in our sample using the H\alpha 10% width and the CaII-8662 line flux as accretion diagnostics. We find that the maximum extent of accretion variability in our sample was reached on timescale of a few days, indicating that rotation could significantly contribute to the variability.

In this thesis, we focus on obtaining and interpreting observational information on (i) the role of multiplicity on the properties of young stars; (ii) the early evolutionary influence of circumstellar disks; and (iii) the nature of accretion in young systems. To facilitate this research, we conducted an extensive multi-epoch high-resolution spectroscopic survey at optical wavelengths (3,200-10,000 A) of ~200 T Tauri stars in the ~2 Myr old Chamaeleon I, and Taurus-Auriga star-forming regions with the Magellan Inamori Kyocera Echelle (MIKE) spectrograph on the Magellan Clay 6.5 m telescope. From the spectroscopic data, we identify eight close binaries and four close triples, of which three and two, respectively, are new discoveries. We find that the multiplicity fraction for Cha I and Tau-Aur are similar to each other, and to the results of field star surveys. The frequency of systems with close companions in our sample is not seen to depend on primary mass or accretion. We probed for evidence of disk braking. We did not see a statistically significant difference between the distribution of rotational velocities with the presence of an inner disk. Also, our findings show that F-K stars in our sample have larger rotational velocities and specific angular momentum than M stars. We also analyzed accretion variability in our sample using the H\alpha 10% width and the CaII-8662 line flux as accretion diagnostics. We find that the maximum extent of accretion variability in our sample was reached on timescale of a few days, indicating that rotation could significantly contribute to the variability.