A powerful local shear instability in weakly magnetized disks. III - Long-term evolution in a shearing sheet

Details A powerful local shear instability in weakly magnetized disks. III - Long-term evolution in a shearing sheet A powerful local shear instability in weakly magnetized disks. III - Long-term evolution in a shearing sheet

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...400..595h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 2, p. 595-609.

Statistics

Computation

157

Accretion Disks, Angular Momentum, Magnetic Field Configurations, Magnetohydrodynamic Stability, Nonlinear Evolution Equations, Computer Animation, Finite Difference Theory, Shear Flow

Scientific paper

The nonlinear evolution of the recently identified accretion disk magnetic shear instability is investigated through a series of numerical simulations. Finite-difference computations of the equations of compressible MHD are carried out on an axisymmetric shearing sheet system with periodic boundary conditions designed to approximate a local region within an accretion disk. Initial field configurations that include some net vertical component evolve into a nonlinear, exponentially growing solution with large poloidal velocities and magnetic fields with energies comparable to the thermal energy density. The stability of a purely azimuthal field configuration is examined, and it is found that nonaxisymmetric instability is present, but with a growth time measured in tens of orbital periods. In general, the most rapid growth occurs for very small radial and azimuthal wavenumbers, leading to coherent magnetic field structure in planes parallel to the disk. It is suggested that this instability is a key ingredient for the generation of magnetic fields in disks.

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