Tilted Disks around Black Holes: A Numerical Parameter Survey for Spin and Inclination Angle. (arXiv:1902.09662v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+White_C/0/1/0/all/0/1">Christopher J. White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quataert_E/0/1/0/all/0/1">Eliot Quataert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blaes_O/0/1/0/all/0/1">Omer Blaes</a>
We conduct a systematic study of the properties of tilted accretion flows
around spinning black holes, covering a range of tilt angles and black hole
spins, using the general-relativistic magnetohydrodynamics code Athena++. The
same initial magnetized torus is evolved around black holes with spins ranging
from 0 to 0.9, with inclinations ranging from 0 degrees to 24 degrees. The
tilted disks quickly reach a warped and twisted shape that rigidly precesses
about the black hole spin axis with deformations in shape large enough to
hinder the application of linear bending wave theory. Magnetized polar outflows
form, oriented along the disk rotation axes. At sufficiently high inclinations
a pair of standing shocks develops in the disks. These shocks dramatically
affect the flow at small radii, driving angular momentum transport. At high
spins they redirect material more effectively than they heat it, reducing the
dissipation rate relative to the mass accretion rate and lowering the radiative
efficiency of the flow.
We conduct a systematic study of the properties of tilted accretion flows
around spinning black holes, covering a range of tilt angles and black hole
spins, using the general-relativistic magnetohydrodynamics code Athena++. The
same initial magnetized torus is evolved around black holes with spins ranging
from 0 to 0.9, with inclinations ranging from 0 degrees to 24 degrees. The
tilted disks quickly reach a warped and twisted shape that rigidly precesses
about the black hole spin axis with deformations in shape large enough to
hinder the application of linear bending wave theory. Magnetized polar outflows
form, oriented along the disk rotation axes. At sufficiently high inclinations
a pair of standing shocks develops in the disks. These shocks dramatically
affect the flow at small radii, driving angular momentum transport. At high
spins they redirect material more effectively than they heat it, reducing the
dissipation rate relative to the mass accretion rate and lowering the radiative
efficiency of the flow.
http://arxiv.org/icons/sfx.gif
