Black Hole Astrophysics : Magnetohydrodynamics on the Kerr Geometry

This work is dedicated to the astrophysics of rotating black holes. The main topic concerns accretion physics in the regime of General Relativistic Magnetohydrodynamics (GRMHD). The behavior of non-radiative accretion flows and outflows on the Kerr space-time is analyzed. Basic equations of conservative GRMHD and aspects of numerical schemes are presented. Relativistic codes and astrophysical simulations validate numerical schemes. A synopsis gives requirements for a robuste GRMHD code. Further developments in GRMHD research are investigated. Another part deals with radiation from accretion disks. Relativistically broadened emission lines from active galactic nuclei and X-ray binaries are calculated by relativistic ray tracing. A new model - based on truncated standard disks - is presented that considers radial drift in accretion flows. Emission lines serve as diagnostic tools to compare parameter studies. Thereby, a classification scheme by line morphology was found: A line profile is triangular, double-horned, bumpy, shoulder-like or double-peaked. Both parts of the work can be connected in further research: results from GRMHD simulations e.g. the velocity field of the flow serve as an input for Kerr ray tracing. Then, realistic spectra are feasible that originate from the vicinity of black holes.

Level thesis:degree_level

thesis.doctoral

Grantor dc:publisher

Universität Heidelberg

Year

2004

Author dc:creator

• Müller, Andreas

Contributors dc:contributor

• Camenzind, Max

Repository record source_url

http://www.ub.uni-heidelberg.de/archiv/5217

OAI identifier oai:identifier

oai:archiv.ub.uni-heidelberg.de:5217