<> "The repository administrator has not yet configured an RDF license."^^ . <> . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation"^^ . "In this thesis, the formation of relativistic jets is investigated by means of special relativistic magnetohydrodynamic simulations and synchrotron radiative transfer. Our results show that the magnetohydrodynamic jet self-collimation paradigm can also be applied to the relativistic case. In the first part, jets launched from rotating hot accretion disk coronae are explored, leading to well collimated, but only mildly relativistic flows. Beyond the light-cylinder, the electric charge separation force balances the classical trans-field Lorentz force almost entirely, resulting in a decreased efficiency of acceleration and collimation in comparison to non-relativistic disk winds. In the second part, we examine Poynting dominated flows of various electric current distributions. By following the outflow for over 3000 Schwarzschild radii, highly relativistic jets of Lorentz factor 8 and half-opening angles below 1 degree are obtained, providing dynamical models for the parsec scale jets of active galactic nuclei. Applying the magnetohydrodynamic structure of the quasi-stationary simulation models, we solve the relativistically beamed synchrotron radiation transport. This yields synthetic radiation maps and polarization patterns that can be used to confront high resolution radio and (sub-) mm observations of nearby active galactic nuclei. Relativistic motion together with the helical magnetic fields of the jet formation site imprint a clear signature on the observed polarization and Faraday rotation. In particular, asymmetries in the polarization direction across the jet can disclose the handedness of the magnetic helix and thus the spin direction of the central engine. Finally, we show first results from fully three-dimensional, high resolution adaptive mesh refinement simulations of jet formation from a rotating magnetosphere and examine the jet stability. Relativistic field-line rotation leads to an electric charge separation force that opposes the magnetic Lorentz force, such that we obtain an increased stability of relativistic flows. Accordingly, the non-axisymmetric modes applied to the field-line foot-points saturate quickly, with no signs of enhanced dissipation or disruption near the jet launching site."^^ . "2011" . . . . . . . . "Oliver Joachim Georg"^^ . "Porth"^^ . "Oliver Joachim Georg Porth"^^ . . . . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (PDF)"^^ . . . "thesis.pdf"^^ . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (Other)"^^ . . . . . . "indexcodes.txt"^^ . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (Other)"^^ . . . . . . "lightbox.jpg"^^ . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (Other)"^^ . . . . . . "preview.jpg"^^ . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (Other)"^^ . . . . . . "medium.jpg"^^ . . . "Formation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation (Other)"^^ . . . . . . "small.jpg"^^ . . "HTML Summary of #12714 \n\nFormation of Relativistic Jets : Magnetohydrodynamics and Synchrotron Radiation\n\n" . "text/html" . . . "520 Astronomie"@de . "520 Astronomy and allied sciences"@en . .