Gravitating discs around black holes

Abstract

Fluid discs and tori around black holes are discussed within different approaches and with the emphasis on the role of disc gravity. First reviewed are the prospects of investigating the gravitational field of a black hole--disc system by analytical solutions of stationary, axially symmetric Einstein's equations. Then, more detailed considerations are focused to middle and outer parts of extended disc-like configurations where relativistic effects are small and the Newtonian description is adequate. Within general relativity, only a static case has been analysed in detail. Results are often very inspiring, however, simplifying assumptions must be imposed: ad hoc profiles of the disc density are commonly assumed and the effects of frame-dragging and completely lacking. Astrophysical discs (e.g. accretion discs in active galactic nuclei) typically extend far beyond the relativistic domain and are fairly diluted. However, self-gravity is still essential for their structure and evolution, as well as for their radiation emission and the impact on the environment around. For example, a nuclear star cluster in a galactic centre may bear various imprints of mutual star--disc interactions, which can be recognised in observational properties, such as the relation between the central mass and stellar velocity dispersion.

Accepted for publication in CQG; high-resolution figures will be available from http://www.iop.org/EJ/journal/CQG

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• Self-gravitating razor-thin disks around black holes via multi-hole seeds
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• Selected Chapters on Active Galactic Nuclei as Relativistic Systems
• Stability aspects of relativistic thin magnetized disks
• Stability of general relativistic Miyamoto-Nagai galaxies
• Interior potential of a toroidal shell from pole values
• Lensing by black holes within astrophysical environments
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