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In a previous work, Ulysses data was analyzed to build a completeaxisymmetric MHD solution for the solar wind at minimum including rotation andthe initial flaring of the solar wind in the low corona. This model has someproblems in reproducing the values of magnetic field at 1 AU despite thecorrect values of the velocity. Here, we intend to extend the previous analysisto another type of solutions and to improve our modelling of the wind from thesolar surface to 1 AU. We compare the previous results to those obtained with afully helicoidal model and construct a hybrid model combining both previoussolutions, keeping the flexibility of the parent models in the appropriatedomain. From the solar surface to the Alfven, point, a three component solutionfor velocity and magnetic field is used, reproducing the complex wind geometryand the well-known flaring of the field lines observed in coronal holes. Fromthe Alfven radius to 1 AU and further, the hybrid model keeps the latitudinaldependences as flexible as possible, in order to deal with the sharp variationsnear the equator and we use the helicoidal solution, turning the poloidalstreamlines into radial ones. Despite the absence of the initial flaring, thehelicoidal model and the first hybrid solution suffer from the same low valuesof the magnetic field at 1 AU. However, by adjusting the parameters with asecond hybrid solution, we are able to reproduce both the velocity and magneticprofiles observed by Ulysses and a reasonable description of the low corona,provided that a certain amount of energy deposit exists along the flow. Thepresent paper shows that analytical axisymmetric solutions can be constructedto reproduce the solar structure and dynamics from 1 solar radius up to 1 AU.Comment: 12 pages, 16 figure

Application of a MHD hybrid solar wind model with latitudinal dependences to ULYSSES data at minimum