Numerical simulation of X-ray-heated winds in Seyfert galaxies. I - The case of zero angular momentum

Details Numerical simulation of X-ray-heated winds in Seyfert galaxies. I - The case of zero angular momentum Numerical simulation of X-ray-heated winds in Seyfert galaxies. I - The case of zero angular momentum

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...402..109b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 402, no. 1, p. 109-124.

Astronomy and Astrophysics

Astrophysics

60

Angular Momentum, Cooling Flows (Astrophysics), Digital Simulation, Hydrodynamic Equations, Seyfert Galaxies, X Ray Astronomy, Active Galactic Nuclei, Boundary Conditions, Line Spectra, Stellar Winds

Scientific paper

Numerical hydrodynamics simulations are presented of X-ray heated winds believed to form the 'mirrors' which reflect light from obscured Seyfert galaxy nuclei into our line of sight. Above a likely range of parameters, it is shown that steady state flows are created when a cool torus surrounds an AGN. Some of the mass evaporated off the inner edge of the torus is captured by the central gravitational well, while the rest is driven off in a warm wind. When the central gravity is strong relative to the radiative heating rate, i.e., L/L(E) is small, nearly all the injected matter is captured. When the gravity is weaker, a given combination of heating rate and injected pressure leads to a maximum mass loss rate; when the rate at which mass is injected exceeds this amount, the excess is captured. The dividing line between these two cases comes at L/L(E) = about 0.08.

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