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We study the correlation heights, which indicate the formation height ofExtreme Ultraviolet (EUV) lines in an active region using observations from theEUV Imaging Spectrometer (EIS) and Solar Optical Telescope (SOT) on board\emph{Hinode}. The nonlinear force-free field (NLFFF) optimization method isadopted to extrapolate the 3D magnetic fields to higher layers. Threesubregions with different characteristics are selected in the active region forthis study. The results show that the formation heights in different subregionsvary with their different magnetic fields or velocity patterns. After solvingthe line blending problem between the He {\sc \romannumeral 2} 256.32 \AA andSi {\sc \romannumeral 10} 256.37 \AA lines by the double Gaussian curvefitting, we find that the transition region lies higher in a strong magneticarea. In a pre-flare heating area there possibly exist multithermal loops asimplied by comparing the Doppler velocity and the magnetic field on the solardisk.

Formation Heights of Extreme Ultraviolet Lines in an Active Region Derived by Correlation of Doppler Velocity and Magnetic Field