  Measurements of the stellar coronal magnetic field are of great importance in
understanding the stellar magnetic activity, yet the measurements have been
extremely difficult. Recent studies proposed a new method of magnetic field
measurements based on the magnetic-field-induced-transition (MIT) of the
Fe~{\sc{x}} ion. Here we construct a series of stellar coronal
magnetohydrodynamics (MHD) models and synthesize several Fe~{\sc{x}} emission
lines at extreme-ultraviolet wavelengths, and then diagnose the magnetic field
strength at the bases of the coronae using the MIT technique. Our results show
that the technique can be applied to some stars with magnetic fields more than
three times higher than that of the Sun at solar maximum. Furthermore, we
investigate the uncertainty of the derived magnetic field strength caused by
photon counting error and find that a signal-noise ratio of $\sim$50 for the
Fe~{\sc{x}} 175 {\AA}~line is required to achieve effective measurements of the
stellar coronal magnetic field.
