Abstract
Non-axial perturbations of a protostellar disk possessing vertical and azimuthal magnetic-field components are studied in the framework of Hall magnetohydrodynamics. The convective transport of the magnetic field by the Hall current leads to instability of fluctuations within a limited interval of wave numbers. The fundamental possibility of the existence of Hall instability in a medium that does not contain an inhomogeneous density distribution, which has not been discussed earlier, is demonstrated. The dependence of the instability increment on both the plasma parameter β and the degree of ionization of the protostellar material are analyzed. Possible consequences for weakly ionized astrophysical disks are discussed.
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