Observational data provided by Voyager 1 and Voyager 2 spacecraft ahead of the heliospheric termination shock (TS) and in the heliosheath require considerate reassessment of theoretical models of the solar wind (SW) interaction with the magnetized interstellar medium (LISM). The TS asymmetry observed by Voyagers can be attributed to the combination of 3D, time-dependent behavior of the SW and by the action of the ISMF. It is clear, however, that the ISMF alone can account for the TS asymmetry of about 10 AU only if it is unexpectedly strong (greater than 4 microgauss). I will analyze the consequences of such magnetic fields for the neutral hydrogen deflection in the inner heliosphere from its original direction in the unperturbed LISM. I will also discuss the conditions for the 2-3 kHz radio emission, which is believed to be generated in the outer heliosheath beyond the heliopause, and analyze the possible location of radio emission sources under the assumption of strong magnetic field. A new model of the solar cycle influence on the distribution of the plasma quantities and magnetic field will be described. The quality of the physical model is crucial when we need to address modern observational and theoretical challenges. I will show the results of the comparison between our MHD-kinetic and 5-fluid models. The importance will be discussed of realistic, based on observations, boundary conditions in the solar wind.