We study the stability of a model of magnetized accretion disk, in which outflows play a significant role in driving the inflow, and magnetic field is generated by a dynamo operating in the disk. We present a local and linear analysis of the stability in the presence of self-gravity and winds. The numerical results show the model with self-gravity is unstable in all parts, while in a model without self-gravity, instability can be observed only in regions near the central body. Eventually, the effect of wind cooling on the model stability was discussed. According to the results, in systems without self-gravity, wind cooling can help the system towards stability, but in the presence of self-gravity, it is shown that our model will remain unstable in all regions. Comparison of these result with observational evidence shows that this model can be suitable for the explaining the behavior of the disks surrounding young stellar objects
