Self-similar structure of resistive ADAFs with outflow and large-scale magnetic field
arXiv:2004.14757 · doi:10.1017/pasa.2020.14
Abstract
The observations and simulations have revealed that large-scale magnetic field and outflows can exist in the inner regions of an advection-dominated accretion disc where the resistive diffusion may also be important. In the present paper, the roles of large-scale magnetic field and outflows in the structure of resistive advection-dominated accretion discs are explored by assuming that the accretion flow is radially self-similar. In the non-ideal magnetohydrodynamic (MHD) approximation, the results show that the angular velocity is always sub-Keplerian when both the outflow and the large-scale magnetic field are taken into account. A stronger toroidal field component leads to faster rotation, while the disc rotates with faster rate if the vertical field component is weaker. The increase of magnetic diffusivity causes the infall velocity to be close to Keplerian velocity. Although the previous studies in the ideal MHD approximation have shown that the disc temperature decreases due to the vertical field component, we find that the effect of vertical field component on the temperature of a resistive disc depends on the magnetic diffusivity. When the magnetic diffusivity is high, the more efficient mechanism for decreasing the disc temperature can be the outflows, and not the large-scale magnetic field. In such a limit of the magnetic diffusivity, the components of the large-scale magnetic field enhance the gas temperature. The increase of temperature can lead to heating and acceleration of the electrons and help us to explain the origin of phenomena such as the flares in Sgr A*. On the other hand, the infall velocity in such a limit rises as the temperature increases, and therefore the surface density falls to too low values. Any change in the density profile can alter the structure and the emitted spectrum of disc.
13 pages, 4 figures
References in corpus (24)
- The Influence of Magnetic Field Geometry on the Evolution of Black Hole Accretion Flows: Similar Disks, Drastically Different Jets
- MHD simulations of the magnetorotational instability in a shearing box with zero net flux. II. The effect of transport coefficients
- Impact of dimensionless numbers on the efficiency of MRI-induced turbulent transport
- Numerical Simulation of Hot Accretion Flows (III): Revisiting wind properties using trajectory approach
- A Constant Spectral Index for Sagittarius A* During Infrared/X-ray Intensity Variations
- 3D Radiation Non-ideal Magnetohydrodynamical Simulations Of The Inner Rim In Protoplanetary Disks
- On the Magnetic Prandtl Number Behavior of Accretion Disks
- Faraday rotation in the jet of M87 inside the Bondi radius: indication of winds from hot accretion flows confining the relativistic jet
- Self-Similar Solution of Hot Accretion Flows with Ordered Magnetic Field and Outflow
- Magnetorotational instability driven dynamos at low magnetic Prandtl numbers
- rHARM: Accretion and Ejection in Resistive GR-MHD
- Angular momentum transport and large eddy simulations in magnetorotational turbulence: the small Pm limit
- Hydrodynamical wind on a magnetized ADAF with thermal conduction
- Radiation hydrodynamics simulations of wide-angle outflows from super-critical accretion disks around black holes
- The large-scale magnetic field of a thin accretion disk with outflows
- Axisymmetric Magnetorotational Instability in Viscous Accretion Disks
- Impact of convection and resistivity on angular momentum transport in dwarf novae
- Hot accretion with outflow and thermal conduction
- On the wind production from hot accretion flows with different accretion rates
- Viscous and resistive accretion flows with radially self-similar and outflows
- Structure of a hot accretion flow in the presence of outflow and convection with large ordered magnetic field
- Global multifluid simulations of the magnetorotational instability in radially stratified protoplanetary disks
- The effects of toroidal magnetic field on the vertical structure of hot accretion flows
- Large resistivity in numerical simulations of radially self-similar outflows