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Magnetic field diagnostics of the transition region from the chromosphere tothe corona faces us with the problem that one has to apply extreme UVspectro-polarimetry. While for coronal diagnostic techniques already existthrough infrared coronagraphy above the limb and radio observations on thedisk, for the transition region one has to investigate extreme UV observations.However, so far the success of such observations has been limited, but thereare various projects to get spectro-polarimetric data in the extreme UV in thenear future. Therefore it is timely to study the polarimetric signals we canexpect for such observations through realistic forward modeling.  We employ a 3D MHD forward model of the solar corona and synthesize theStokes I and Stokes V profiles of C IV 1548 A. A signal well above 0.001 inStokes V can be expected, even when integrating for several minutes in order toreach the required signal-to-noise ratio, despite the fact that the intensityin the model is rapidly changing (just as in observations). Often thisvariability of the intensity is used as an argument against transition regionmagnetic diagnostics which requires exposure times of minutes. However, themagnetic field is evolving much slower than the intensity, and thus whenintegrating in time the degree of (circular) polarization remains ratherconstant. Our study shows the feasibility to measure the transition regionmagnetic field, if a polarimetric accuracy on the order of 0.001 can bereached, which we can expect from planned instrumentation.

Magnetic field diagnostics and spatio-temporal variability of the solar transition region