  Measurements of the magnetic field in the stellar coronae are extremely
difficult. Recently, it was proposed that the magnetic-field-induced transition
(MIT) of the Fe X 257 {\AA} line can be used to measure the coronal magnetic
field of the Sun. We performed forward modeling with a series of global stellar
magnetohydrodynamics models to investigate the possibility of extending this
method to other late-type stars. We first synthesized the emissions of several
Fe X lines for each stellar model, then calculated the magnetic field strengths
using the intensity ratios of Fe X 257 {\AA} to several other Fe X lines based
on the MIT theory. Finally, we compared the derived field strengths with those
in the models, and concluded that this method can be used to measure at least
the magnetic field strengths at the coronal bases of stars with a mean surface
magnetic flux density about one order of magnitude higher than that of the Sun.
Our investigation suggests the need of an extreme ultraviolet spectrometer to
perform routine measurements of the stellar coronal magnetic field.
