Abstract
The structure and stability of a magnetized accretion disk are numerically examined with anomalous viscosity. The temperature, surface density and radial velocity all decrease with increasing radius r. The results show that the existence of the magnetic field B has an impact on the structure of the disk, which directly results in the variation of the growth rate and the damping rate of the unstable and stable modes. For Inward-moving mode, the magnetic field greatly enhances the instability at short wavelength and acts as a factor of stability at long wavelength. The growth rate of outward-moving unstable mode decreases, while the damping rate of thermally stable mode increases significantly owing to the magnetic field.
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Zhou, Ap., Liu, Hf. & Gao, Jx. Structure and stability of magnetized accretion disks with anomalous viscosity. Astrophys Space Sci 348, 337–343 (2013). https://doi.org/10.1007/s10509-013-1583-2
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DOI: https://doi.org/10.1007/s10509-013-1583-2