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We have previously found a temperature-dependent upflow in the dimming regionfollowing a coronal mass ejection (CME) observed by the {\it Hinode} EUVImaging Spectrometer (EIS). In this paper, we reanalyzed the observations alongwith previous work on this event, and provided boundary conditions formodeling. We found that the intensity in the dimming region dramatically dropswithin 30 minutes from the flare onset, and the dimming region reaches theequilibrium stage after $\sim$1 hour later. The temperature-dependent upflowswere observed during the equilibrium stage by EIS. The cross sectional area ofthe fluxtube in the dimming region does not appear to expand significantly.From the observational constraints, we reconstructed the temperature-dependentupflow by using a new method which considers the mass and momentum conservationlaw, and demonstrated the height variation of plasma conditions in the dimmingregion. We found that a super radial expansion of the cross sectional area isrequired to satisfy the mass conservation and momentum equations. There is asteep temperature and velocity gradient of around 7 Mm from the solar surface.This result may suggest that the strong heating occurred above 7 Mm from thesolar surface in the dimming region. We also showed that the ionizationequilibrium assumption in the dimming region is violated especially in thehigher temperature range.

1D Modeling for Temperature-Dependent Upflow in the Dimming Region Observed by Hinode/EIS