Structure and stability of a thin protostar disk with anomalous viscosity

Abstract

The structure of a thin protostar disk has been investigated in the frame of anomalous magnetic viscosity prescription. The numerical results reveal that, the dynamical behavior of the disk with anomalous magnetic viscosity model is different from one with the well-known α-prescription, and the former can reveal the real behavior of the disk.The linear stability of this disk has also been examined under the short wavelength approximation (kr 1). It shows that the I-mode, O-mode and thermal mode are unstable in the inner and outer region of the thin protostar disk, on the contrary, viscous mode is stable. The growth time scale for these instabilities in the outer region are shorter than ones in the inner.

The radial–azimuthal instability of accretion disk with anomalous viscosity

“…Subsequently, Chen and Taam and Wu et al got similar results, although some additional terms, such as causally limited viscosity [12] and radial viscous force [13], respectively, were included. After the anomalousviscosity model was presented in 2002, Yao and Li and Chen and Liu analyzed the instabilities of the accretion disk adopted the Li and Zhang's viscosity prescription by numerical simulations [14][15][16][17][18][19][20].…”