The effect of heat conduction on the interaction of disk and corona around black holes

Abstract

Heat conduction plays an important role in the balance between heating and cooling in many astrophysical objects, e.g. cooling flows in clusters of galaxies. Here we investigate the effect of heat conduction on the interaction between a cool disk and a hot corona around black holes. Using the one-radial-zone approximation, we study the vertical structure of the disk corona and derive evaporation and coronal mass flow rates for various reduced thermal conductivities. We find lower evaporation rates and a shift in the evaporation maxima to smaller radii. This implies that the spectral state transition occurs at a lower mass flow rate and a disk truncation closer to the black hole. Reductions of thermal conductivity are thought to be magnetically caused and might vary from object to object by a different configuration of the magnetic fields.

arXiv commentaccepted for publication in A & A, 5 pages

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Cited by in corpus (11)

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• Anatomy of the AGN in NGC 5548 VIII. XMM-Newton's EPIC detailed view of an unexpected variable multilayer absorber
• The Dependence of Spectral State Transition and Disk Truncation on Viscosity Parameter $α
• Application of the Disk Evaporation Model to AGNs
• Broad iron emission lines in Seyfert Galaxies - re-condensation of gas onto an inner disk below the ADAF
• Disk-Evaporation Fed Corona: Structure and Evaporation Feature with Magnetic Field
• Analytical Model of Disk Evaporation and State Transitions in Accreting Black Holes
• Low heat conduction in white dwarf boundary layers?
• Kelvin-Helmholtz Instability at the interface of a disc-corona system
• Simple interpretation of the seemingly complicated X-ray spectral variation of NGC 5548
• Magnetic seed generation by plasma heat flux in accretion disks