  According to the standard thin disc theory, it is predicted that the
radiation-pressure-dominated inner region of a thin disc is thermally unstable,
while observations suggest that it is common for a thin disc of more than 0.01
Eddington luminosity to be in a thermally stable state. Previous studies have
suggested that magnetically driven winds have the potential to suppress
instability. In this work, we implement one-dimensional global simulations of
the thin accretion disc to study the effects of magnetically driven winds on
thermal instability. The winds play a role in transferring the angular momentum
of the disc and cooling the disc. When the mass outflow rate of winds is low,
the important role of winds is to transfer the angular momentum and then
shorten the outburst period. When the winds have a high mass outflow rate, they
can calm down the thermal instability. We also explore the parameter space of
the magnetic field strength and the mass loading parameter.
