Global ETD Search
Search theses and dissertations gathered from participating repositories worldwide. Every result links back to the library that holds it. No account is needed.
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Showing 1 to 9 of 9 for “"Thermal pressure"”.
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The role of magnetic braking and ambipolar diffusion in the formation of interstellar cloud cores and protostars
… in astrophysics. Magnetic fields, which dominate thermal-pressure as a source of support against self-gravity in interstellar molecular clouds, are an important regulator of star-formation. We study the formation and contraction of fragments (or cores) in isothermal, rotating, magnetic molecular …
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Star formation in the presence of magnetic fields: Molecular cloud core formation and dynamical contraction due to ambipolar diffusion; a simulation with axial symmetry
… imply that well-ordered magnetic fields dominate thermal pressure in supporting these objects against self-gravity. The magnetic force is transferred to the neutrals through collisions with ions. Because the degree of ionization drops as the density increases, redistribution of the mass-to-flux …
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On the evolution of gaseous haloes in cosmological simulations of galaxy formation
… velocities, leading to a doubling of non-thermal pressure support. With the FABLE suite, I studied how the hydrostatic mass bias and turbulent pressure support level in galaxy clusters change as they undergo major mergers and are host to powerful feedback episodes. I found that clusters …
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On physical processes occurring in the hydrodynamic and magnetohydrodynamic astrophysical and laboratory flows
… ball of heavy neutrinos, supported by degeneracy pressure, does exist in the vicinity of the active galactic nuclei, it will cause a bump in IR region of the emitted spectrum which is observed for several AGN (Malkan, 1989). We also find that if the bump at ~ 1000K in the typical radio loud quasar …
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Gamma-Ray Burst Early Optical Afterglow Modelling
… would suggest that the ejecta is driven by thermal pressure. Finally we consider how inhomogeneities present in the outflow can lead to variations in the very early afterglow. Considering small gradi- ent in the ejecta density profile modifies the rising index of the afterglow and can be …
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Mass profiles of clusters of galaxies : a comparison of X-ray and weak lensing observations
… et al., 2010). The temperature, gas density, pressure, gas fraction profiles and their relation to the cluster morphology are also examined. We find that slopes of X-ray pressure and mass profiles vary with cluster morphology. Specifically, clusters with lower third-order power ratios P3=P0 …
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The Role of MHD Waves and Ambipolar Diffusion in the Formation of Interstellar Cloud Cores and Protostars
… of cloud cores due to ambipolar diffusion in isothermal, magnetic molecular clouds in the presence of MHD waves. The model clouds are initially in exact equilibrium states, with magnetic, thermal-pressure, and wave-pressure forces balancing self-gravity. An energy equation for MHD waves in a …
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Exploring Galaxy Clusters and Groups with Cosmological Simulations
… to a combination of factors, including non-thermal pressure support provided by kinetic motions in the intracluster gas and the effects of non-gravitational physics such as AGN feedback. I also find a significant variation in the scatter about the relations with changing halo mass and …