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Winds are commonly observed in luminous active galactic nuclei (AGNs). Aplausible model of those winds is magnetohydrodynamic (MHD) disc winds. In thecase of disc winds from a thin accretion disc, isothermal or adiabaticassumption is usually adopted in such MHD models. In this work we performtwo-dimensional MHD simulations implementing different thermal treatments(isothermal, adiabatic and radiative) to study their effects on winds from athin accretion disc. We find that both the isothermal model and the adiabaticmodel overestimate the temperature, underestimate the power of disc winds, andcannot predict the local structure of the winds, compared to the resultsobtained by solving the energy equation with radiative cooling and heating.Based on the model with radiative cooling and heating, the ionizationparameter, the column density and the velocity of the disc winds have beencompared to the observed ultrafast outflows (UFOs). We find that in oursimulations the UFOs can only be produced inside hundreds of Schwarzschildradius. At much larger radii, no UFOs are found. Thus, the pure MHD windscannot interpret all the observed UFOs.

Magnetically driven accretion disc winds: the role of gas thermodynamics and comparison to ultra-fast outflows