“School of Astronomy”
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| Paper IPM / Astronomy / 14928 |
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| Abstract: | |||||
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We investigate the properties of a hot accretion flow bathed in a poloidal magnetic field. We consider an
axisymmetric viscous-resistive flow in the steady-state configuration. We assume that the dominant mechanism of
energy dissipation is due to turbulence viscosity and magnetic diffusivity. A certain fraction of that energy can be
advected toward the central compact object. We employ the self-similar method in the radial direction to find a
system of ODEs with just one varible, ø in the spherical coordinates. For the existence and maintenance of a purely
poloidal magnetic field in a rotating thick disk, we find that the necessary condition is a constant value of angular
velocity along a magnetic field line. We obtain an analytical solution for the poloidal magnetic flux. We explore
possible changes in the vertical structure of the disk under the influences of symmetric and asymmetric magnetic
fields. Our results reveal that a polar magnetic field with even symmetry about the equatorial plane makes the disk
vertically thin. Moreover, the accretion rate decreases when we consider a strong magnetic field. Finally, we notice
that hot magnetized accretion flows can be fully advected even in a slim shape.
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