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Using one-arcsecond-slit scan observations from the Hinode/EUV ImagingSpectrometer (EIS) on 05 February 2007, we find the plasma outflows in the openand expanding coronal funnels at the eastern boundary of AR 10940. The Dopplervelocity map of Fe XII 195.120 A shows that the diffuse close-loop system to bemostly red-shifted. The open arches (funnels) at the eastern boundary of ARexhibit blue-shifts with a maximum speed of about 10-15 km/s. This impliesoutflowing plasma through these magnetic structures. In support of theseobservations, we perform a 2D numerical simulation of the expanding coronalfunnels by solving the set of ideal MHD equations in appropriate VAL-III Cinitial temperature conditions using the FLASH code. We implement a rarefiedand hotter region at the footpoint of the model funnel, which results in theevolution of slow plasma perturbations propagating outward in the form ofplasma flows. We conclude that the heating, which may result from magneticreconnection, can trigger the observed plasma outflows in such coronal funnels.This can transport mass into the higher corona, giving rise to the formation ofthe nascent solar wind.

On Thermal-Pulse-Driven Plasma Flows in Coronal Funnels as Observed by Hinode/EUV Imaging Spectrometer (EIS)