Radiative cooling effects on black hole hot accretion flows around the sub-Bondi radius
arXiv:2604.13762 · doi:10.1051/0004-6361/202557811
Abstract
It is difficult to implement numerical simulations on a region extending from the vicinity of a black hole to the Bondi radius. Most previous numerical simulations have primarily concentrated on the region close to the black hole. They found that strong winds can be generated in the hot accretion flows near the black hole, and that radiative cooling significantly affects the strength of these winds. However, the effects of radiative cooling on the production and properties of winds around the Bondi radius remain unclear. In this paper, we perform two-dimensional magnetohydrodynamic simulations to study the impact of radiative cooling on the dynamics and wind production in hot accretion flows around the sub-Bondi radius. As the increase of mass accretion rate, radiative cooling gradually becomes strong, resulting in a reduction in the thickness of the accretion disk (defined as the accretion flows within the density scale height). Based on the Høiland criterion, we find that within the accretion disk, the region of convective stability accounts for 55 - 62 %, and therefore the accretion flows are marginally stable in convective stability. In the runs with weak radiative cooling, the winds play a significant role in the inward decrease of the mass inflow rate. In the runs with strong radiative cooling, the mass outflow rate of winds is significantly reduced and then the inward decrease of the mass inflow rate is mainly attributed to turbulence driven by magnetorotational instability and convection. Radiative cooling has the potential to suppress accretion processes and reduce the power of winds.
15 pages, 23 figures, accepted by A&A
References in corpus (46)
- Advection-Dominated Accretion: A Self-Similar Solution
- PLUTO: a Numerical Code for Computational Astrophysics
- Hot Accretion Flows Around Black Holes
- Efficient Generation of Jets from Magnetically Arrested Accretion on a Rapidly Spinning Black Hole
- Nuclear Activity in Nearby Galaxies
- Advection-Dominated Accretion: Self-Similarity and Bipolar Outflows
- The ATLAS3D project - III. A census of the stellar angular momentum within the effective radius of early-type galaxies: unveiling the distribution of Fast and Slow Rotators
- Thermal Equilibria of Accretion Disks
- GRMHD Simulations of Magnetized Advection Dominated Accretion on a Non-Spinning Black Hole: Role of Outflows
- The PLUTO Code for Adaptive Mesh Computations in Astrophysical Fluid Dynamics
- A Global Three Dimensional Radiation Magneto-hydrodynamic Simulation of Super-Eddington Accretion Disks
- Self-Similar Accretion Flows with Convection
- Hydrodynamical Non-radiative Accretion Flows in Two-Dimensions
- Radiatively Inefficient Accretion in Nearby Galaxies
- Angular Momentum Transport by MHD Turbulence in Accretion Disks: Gas Pressure Dependence of the Saturation Level of the Magnetorotational Instability
- Dissecting X-ray-emitting Gas around the Center of our Galaxy
- The Dynamical Structure of Nonradiative Black Hole Accretion Flows
- The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets
- Numerical Simulation of Hot Accretion Flows (II): Nature, Origin, and Properties of Outflow and Their Possible Observational Applications
- Magnetohydrodynamical Non-radiative Accretion Flows in Two-Dimensions
- Super-Eddington Accretion Disks around Supermassive black Holes
- Numerical Simulation of Hot Accretion Flows (III): Revisiting wind properties using trajectory approach
- Assessing Quantitative Results in Accretion Simulations: From Local to Global
- Two-dimensional models of hydrodynamical accretion flows into black holes
- Global Evolution of an Accretion Disk with Net Vertical Field: Coronal Accretion, Flux Transport, and Disk Winds
- Magnetohydrodynamical Accretion Flows: Formation of Magnetic Tower Jet and Subsequent Quasi-Steady State
- A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions
- Radiatively Inefficient Accretion: Breezes, Winds and Hyperaccretion
- Testing Convergence for Global Accretion Disks
- Luminous hot accretion disks
- On the Thermal Stability of Radiation Dominated Accretion Disks
- Rotating Accretion Flows: From Infinity to the Black Hole
- General Relativistic Magnetohydrodynamic Simulations of the Hard State as a Magnetically-Dominated Accretion Flow
- The large scale magnetic fields of advection dominated accretion flows
- A new equilibrium torus solution and GRMHD initial conditions
- Magneto-hydrodynamical Numerical simulation of wind production from black hole hot accretion flows at very large radii
- Thermal stability of thin disk with magnetically driven winds
- Active Galactic Nuclei Feedback in an Elliptical Galaxy with the Most Updated AGN Physics (II): High-Angular Momentum Case
- Low density, radiatively inefficient rotating-accretion flow onto a black hole
- GRRMHD Simulations of MAD Accretion Disks Declining from Super-Eddington to Sub-Eddington Accretion Rates
- MACER improved: AGN feedback computed in rotating early-type galaxies at high resolution
- Transition of BH feeding from the quiescent regime into star-forming cold disk regime
- On the wind production from hot accretion flows with different accretion rates
- Effects of anisotropic thermal conduction on wind properties in hot accretion flow
- Observational evidence for AGNs feedback at parsec scale
- Energetics in MRI driven Turbulence