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We present evidence that transition region red-shifts are naturally producedin episodically heated models where the average volumetric heating scale heightlies between that of the chromospheric pressure scale height of 200 km and thecoronal scale height of 50 Mm. In order to do so we present results from 3d MHDmodels spanning the upper convection zone up to the corona, 15 Mm above thephotosphere. Transition region and coronal heating in these models is due boththe stressing of the magnetic field by photospheric and convection `zonedynamics, but also in some models by the injection of emerging magnetic flux.

On red shifs in the transition region and corona