  It is believed that the spectral state transitions of the outbursts in X-ray
binaries (XRBs) are triggered by the rise of the mass accretion rate due to
underlying disc instabilities. Recent observations found that characteristics
of disc winds are probably connected with the different spectral states, but
the theoretical underpinnings of it are highly ambiguous. To understand the
correlation between disc winds and the dynamics of the accretion flow, we have
performed General Relativistic Magneto-hydrodynamic (GRMHD) simulations of an
axisymmetric thin accretion disc with different accretion rates and magnetic
field strengths. Our simulations have shown that the dynamics and the
temperature properties depend on both accretion rates and magnetic field
strengths. We later found that these properties greatly influence spectral
properties. We calculated the average coronal temperature for different
simulation models, which is correlated with high-energy Compton emission. Our
simulation models reveal that the average coronal temperature is
anti-correlated with the accretion rates, which is correlated with the magnetic
field strengths. We also found that the structured component of the disc winds
(Blandford-Payne disc wind) predominates as the accretion rates and magnetic
field strengths increase. In contrast, the turbulent component of the disc
winds ($B_{\rm tor}$ disc wind) predominates as the accretion rates and
magnetic field strengths decrease. Our results suggest that the disc winds
during an outburst in XRBs can only be understood if the magnetic field
contribution varies over time (e.g., MAXI J1820+070).
