On the wind production from hot accretion flows with different accretion rates

Abstract

We perform two-dimensional simulations to study how the wind strength changes with accretion rate. We take into account bremsstrahlung, synchrotron radiation and the Comptonization. We find that when the accretion rate is low, radiative cooling is not important, the accretion flow is hot accretion flow. For the hot accretion flow, wind is very strong. The mass flux of wind can be $\sim 50\%$ of the mass inflow rate. When the accretion rate increases to a value at which radiative cooling rate is roughly equal to or slightly larger than viscous heating rate, cold clumps can form around the equatorial plane. In this case, the gas pressure gradient force is small and wind is very weak. Our results may be useful for the sub-grid model of active galactic nuclear feedback study.

9 pages, 8 figures, accepted by MNRAS

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Cited by in corpus (12)

• Radiative Properties of Magnetically-Arrested Disks
• The Origin of Matter at the Base of Relativistic Jets in Active Galactic Nuclei
• Large-scale Dynamics of Winds Driven by Line Force from a Thin Accretion Disk
• Thermal Equilibrium Solutions of Black Hole Accretion Flows: Outflows VS Advection
• Hot accretion flow around neutron stars
• Self-similar structure of resistive ADAFs with outflow and large-scale magnetic field
• Two-temperature radiative hot accretion flow around neutron stars
• Black holes: accretion processes in X-ray binaries
• Self-similar Solution of Hot Accretion Flow with Thermal Conduction and Anisotropic Pressure
• The width-flux relation of the broad iron line during the state transition of the black hole X-ray binaries
• Thermal Conduction in Clumpy Disks and BLR clouds
• Radiative cooling effects on black hole hot accretion flows around the sub-Bondi radius