On the formation of a quasi-stationary twisted disc after a tidal disruption event
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Abstract
We investigate misaligned accretion discs formed after tidal disruption
events that occur when a star encounters a supermassive black hole. We employ
the linear theory of warped accretion discs to find the shape of a disc for
which the stream arising from the disrupted star provides a source of angular
momentum that is misaligned with that of the black hole. For quasi-steady
configurations we find that when the warp diffusion or propagation time is
large compared to the local mass accretion time and/or the natural disc
alignment radius is small, misalignment is favoured. These results have been
verified using SPH simulations. We also simulated 1D model discs including gas
and radiation pressure. As accretion rates initially exceed the Eddington limit
the disc is initially advection dominated. Assuming the
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1365-2966