Larger black holes in TDEs accrete more material and launch faster winds, with unbound mildly relativistic winds for higher viscosity parameters and bound convective outflows for lower ones.
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2 Pith papers cite this work, alongside 163 external citations. Polarity classification is still indexing.
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UNVERDICTED 2representative citing papers
Magnetic filaments in the solar convection zone form in two stages: a kinematic frozen-in phase at convective cell boundaries followed by a dynamic phase where magnetic pressure alters the flow until kinetic and magnetic energy densities become comparable.
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Hydrodynamical simulation of wind production from hot accretion flows in tidal disruption events
Larger black holes in TDEs accrete more material and launch faster winds, with unbound mildly relativistic winds for higher viscosity parameters and bound convective outflows for lower ones.
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Two stages of magnetic filament formation in the solar convective zone
Magnetic filaments in the solar convection zone form in two stages: a kinematic frozen-in phase at convective cell boundaries followed by a dynamic phase where magnetic pressure alters the flow until kinetic and magnetic energy densities become comparable.