  Recently, it has been proposed that the magnetic-field-induced transition
(MIT) in Fe X can be used to measure coronal magnetic field strengths. Several
techniques, the direct line ratio technique and the weak and strong magnetic
field techniques, are developed to apply the MIT theory to spectroscopic
observations taken by EUV Imaging Spectrometer (EIS) onboard Hinode. However,
the suitability of coronal magnetic field measurements based on the weak and
strong magnetic field techniques has not been evaluated. Besides, temperature
diagnostics is also important for measuring coronal magnetic field based on the
MIT theory, but how to determine the accurate formation temperature of the Fe X
lines from EIS observations still needs investigation. In this study, we
synthesized emissions of several spectral lines from a 3D radiation
magnetohydrodynamic model of a solar active region, and then derived magnetic
field strengths using different methods. We first compared the magnetic field
strengths derived from the weak and strong magnetic field techniques to the
values in the model. Our study suggests that both weak and strong magnetic
field techniques underestimate the coronal magnetic field strength. Then we
developed two methods to calculate the formation temperature of the Fe X lines.
One is based on differential emission measure analyses, and the other is
deriving temperature from the Fe IX and Fe XI line pairs. However, neither of
the two methods can provide temperature determination for accurate coronal
magnetic field measurements as those derived from the Fe X 174/175 and 184/345
{\AA} line ratios. More efforts are still needed for accurate coronal magnetic
field measurements using EIS observations.
