We present solar wind modeling efforts with both magnetohydrodynamic (MHD) and kinetic treatments. An observation-driven MHD model is used to constrain a kinetic solar wind model with anisotropic kappa velocity distribution functions (VDF) for the electrons. Photospheric magnetograms serve as observational input in semi-empirical coronal models for estimating the plasma characteristics up to a heliocentric distance of 0.1AU. A full MHD model is employed for computing the three-dimensional evolution of the solar wind macroscopic variables up to 2AU. The results of the MHD model obtained at 0.1AU serve to constrain the parameters used in an exospheric kinetic solar wind model. The assumption of Maxwell and kappa VDF at the exobase, for protons and electrons respectively, is used to determine the solar wind solution using appropriate boundary conditions, estimated to obtain the best comparison with available observations at the Earth. The kinetic description sheds light on processes such as coronal heating and solar wind acceleration, that naturally appear by inclusion of suprathermal electrons in the model. We are focusing on the profile and variation of solar wind parameters, such as the solar wind speed, temperature and density at 1 AU, on characterizing the slow and fast source regions of the wind and on comparing its features with results of exospheric models in similar conditions. In order to compare MHD and kinetic approaches with observations, we start from similar boundary conditions at the 0.1AU and propagate the global kinetic solution up to 2AU.