Evolutionary Structure of Magnetized Accretion Flow Incorporating Saturated Thermal Conduction

Document Type : Research Paper

Authors

School of Physics, Damghan University, Damghan, Iran

10.22128/ijaa.2026.3224.1243

Abstract

This paper presents a time-dependent model for magnetized, advection-dominated accretion flows (ADAFs) that incorporates non-ideal effects, specifically resistivity and saturated thermal conduction. We apply a self-similar method to transform the full time-dependent magnetohydrodynamic (MHD) equations into a set of coupled ordinary differential equations, enabling us to investigate the evolving radial structure influenced by turbulent viscosity, magnetic diffusivity, and non-local energy transport. The resulting solutions confirm that the flow structure is inherently time-dependent. Numerical results demonstrate that increasing the efficiency of outward energy transport via saturated conduction weakens turbulence, reduces dissipation and temperature, increases density, and reduces the radial infall velocity while increasing the rotational velocity. In contrast, stronger magnetization leads to enhanced magnetic fields, lower temperatures, and faster radial inflow. We further show that the turbulence prescription parameter, which controls the pressure dependence of transport coefficients, significantly influences the balance between magnetic and thermal support. This framework offers a dynamic perspective on magnetized accretion flows, highlighting how non-ideal magnetic effects and conduction regulate the flow structure.

Keywords

References

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Iranian Journal of Astronomy and Astrophysics
Volume 12, Issue 4
February 2026
Pages 311-322

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