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As it was shown by Lallement et al. (2005, 2010) interstellar hydrogen atoms are deflected inside the heliosphere due to global distortion of the heliospheric interface by Interstellar Magnetic Field (IsMF). It was demonstrated that spectral measurements of the backscattered solar Lyman-alpha radiation at 1 AU can be used for remote diagnostic of the hydrogen deflection, and hence, configuration of the interstellar magnetic field. In this work we applied our state-of-art 3D time-dependent kinetic model for calculation of interstellar hydrogen distribution in the heliosphere during full solar cycle. Then we calculated spectral properties of the corresponding backscattered solar Lyman-alpha radiation and obtained the deflection of hydrogen flow exactly as it was done previously by Quemerais et al. (1999) and Lallement et al. (2010) based on analysis of the SOHO/SWAN experimental data. It is shown that deflection of hydrogen atoms inside the heliosphere depends not only on the IsMF, but on the solar parameters as well. We have shown that during solar cycle hydrogen deflection defined from the Lyman-alpha spectral properties at 1 AU changes by 1.2 degree due to local variations of the solar wind and solar radiation parameters. It means that for interpretation of such measurements of Lyman-alpha radiation one needs to take these variations into account. Direction of hydrogen flow obtained from our numerical model is in good agreement with the results presented in Lallement et al. (2010) based on the analysis of SOHO/SWAN data on the Lyman-alpha radiation for 1996 and 2001.