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The slow evolution of the coronal magnetic field is frequently modelled by a sequence to static equiibria. We investigate and compare 5 different methods for studying such an evolution. The coronal magnetic field is slowly stressed by slow photospheric motions. If the loop length is much larger than the loop width then this allows a variety of different approximations to be used. We compare the results using (i) a Magneto-frictional method, (ii) a simple 1D approach, (iii) a linearisation of the MHD equations, (iv) Reduced MHD and finally (v) a full MHD simulation. We investigate when the methods are valid and when they fail.