Gas flows in an Active galactic nuclei. I. Two-phase gas inflow

Abstract

We perform two-dimensional hydrodynamic simulations to study the non-rotating gas flow in the region from 1-1000 parsec. This region connects the galaxy scale and the accretion disk scale. The gas is irradiated by the photons generated by the accretion disk system near the central black hole with $10^8$ solar mass. We assume that the luminosity of the central accretion system is constant and equals to $0.3$ Eddington luminosity. Gas with density higher than $10^{-24}\mathrm{g}\mathrm{c}{\mathrm{m}}^{-3}$ is found to be thermally unstable. Two phase, cold and hot, gas flow will form due to thermal instability. We calculated the ratio of cold gas accretion rate to hot gas accretion rate. This ratio is a function of gas density and generally increases with the increase of gas density. The maximum value of this ratio is $16$, when gas density is $10^{-21}\mathrm{g}\mathrm{c}{\mathrm{m}}^{-3}$. Gas with density lower than $10^{-24}\mathrm{g}\mathrm{c}{\mathrm{m}}^{-3}$ is found to be thermally stable and the gas flow is one-phase. The applications of the results are briefly discussed.

9 pages, 10 figures, accepted by MNRAS

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Cited by in corpus (2)

• Review the possible advective disk structures around a black hole with two-type gas inflows
• Dynamical and thermal properties of the parsec-scale gases spherically accreted onto low luminous active galactic nuclei