Global resistive MHD accretion flows around spinning AGNs: impact of resistivity on MAD state

Abstract

In this study, we investigate the effect of resistivity on the dynamics of global magnetohydrodynamic accretion flows (Res-MHD) around a spinning supermassive black hole. We perform a comparative study of 2D and 3D resistive models around black holes. We examine accretion flow dynamics considering globally uniform resistivity values, ranging from $\sim 0$ to 0.1. During the simulation time of $t\lesssim 1000t_g$, we find that the mass accretion rate is comparable for both the 2D and 3D models. However, as the flow becomes increasingly turbulent, non-axisymmetric effects begin to dominate, resulting in significant differences in the mass accretion rates between the 3D and 2D. All the resistive models in a highly magnetized flow belong to the Magnetically Arrested Disk (MAD) state. We propose an efficient and physically motivated approach to examine the magnetic state by estimating the spatial average plasma beta parameter across the computational domain. We find that when the average plasma beta is close to or below unity $({\beta }_{\text{ave}}\lesssim 1)$, the accretion flow enters the MAD state. Additionally, we find that high-resistivity flow reduces magnetorotational instability (MRI) turbulence in the accretion flow, while the turbulence structures remain qualitatively similar in low-resistivity flows. Moreover, we observe indications of plasmoid formations in low-resistivity flow compared to high-resistivity flow. Furthermore, we do not find a clear relationship between the variability of the accretion rate, magnetic flux, and resistivity. Lastly, our findings suggest that low-resistivity models produce higher power jets than those with higher resistivity.

17 pages, 9 figures, 2 tables; Accepted for publication in ApJ

References in corpus (26)

• First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole
• First Sagittarius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way
• PLUTO: a Numerical Code for Computational Astrophysics
• First M87 Event Horizon Telescope Results. VIII. Magnetic Field Structure near The Event Horizon
• Black hole flares: ejection of accreted magnetic flux through 3D plasmoid-mediated reconnection
• Magnetic Reconnection and Hot Spot Formation in Black Hole Accretion Disks
• Magnetically Arrested Disks and Origin of Poynting Jets: Numerical Study
• Modeling the orbital motion of Sgr A*'s near-infrared flares
• Plasmoid formation in global GRMHD simulations and AGN flares
• Precessing jet nozzle connecting to a spinning black hole in M87
• Flux eruption events drive angular momentum transport in magnetically arrested accretion flows
• A 600 minute near-infrared lightcurve of Sagittarius A*
• Comparison of the ion-to-electron temperature ratio prescription: GRMHD simulations with electron thermodynamics
• The X-ray Flux Distribution of Sagittarius A* as Seen by Chandra
• A Resolution Study of Magnetically Arrested Disks
• Jets, disc-winds and oscillations in general relativistic, magnetically driven flows around black hole
• The Jet-Disk Boundary Layer in Black Hole Accretion
• GRRMHD Simulations of MAD Accretion Disks Declining from Super-Eddington to Sub-Eddington Accretion Rates
• A Possible Model for the Long-Term Flares of Sgr A*
• Two-Temperature GRMHD Simulations of Black Hole Accretion Flows with Multiple Magnetic Loops
• Magnetic Flux Transport in Radiatively Inefficient Accretion Flows and the Pathway towards a Magnetically Arrested Disk
• Can MAD accretion disks launching structured jets explain both GRB and AGN engines? Magnetically arrested accretion disks launching structured jets in application to GRB and AGN engines
• Radiative shock oscillation model for the long-term flares of Sgr A*
• Truncated accretion discs in black hole X-ray binaries: dynamics and variability signatures
• The impact of resistivity on the variability of black hole accretion flows
• Time delays between radio and X-ray and between narrow radio bands of Sgr A* flares in the shock oscillation model

Cited by in corpus (1)

• The azimuthal structure of magnetically arrested disks during flux eruption events