Other
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.2607k&link_type=abstract
American Astronomical Society, HEAD meeting #10, #26.07
Other
Scientific paper
We present three-dimensional hydrodynamical simulations of gas flows in the vicinity of an active galactic nucleus (AGN) powered by a precessing accretion disk. We consider the effects of the radiation force from such a disk on its environment on a relatively large scale (up to 10 pc). We implicitly include the precessing disk by forcing the disk radiation field to precess around a symmetry axis with a given period (P) and a tilt angle (Theta). We study time evolution of the flows irradiated by the disk, and investigate basic dependencies of the flow morphology, mass flux, angular momentum on different combinations of Theta and P. We first consider a simplest form of radiation force i.e., force due to electron scattering, and neglect the forces due to line scattering/absorption. Further, the gas is assumed to be nearly isothermal. We find the gas flow settles into a configuration with two components, (1) an equatorial inflow and (2) a bipolar inflow/outflow with the outflow leaving the system along the poles (the directions of disk normals). However, the flow does not always reach a steady state. The kinetic outflow power and the maximum outflow velocity decrease with increasing Theta. We also find that of the mass inflow rate across the inner boundary does not change significantly with increasing Theta. The general characteristics of the flows are closely related to a combination of P and Theta, but not to P and Theta individually. Our models exhibit helical structures similar to those observed in the weakly collimated outflows. As a next phase of our investigation we consider 3D effects of the line force and radiative cooling/heating on the flow. We finish with presenting preliminary results from these more advanced calculations.
Kurosawa Ryuichi
Proga Daniel
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