As the Sun moves through the local interstellar medium (LISM) it emits charged particles creating the heliosphere. Since we cannot see the heliosphere directly, as this can be done for some astrospheres, determining its structure is a fundamental question to be answered by theoretical models. We apply the existing knowledge of the observed and theoretically prescribed LISM and solar wind turbulence to estimate their ability to destroy the heliotail structure and ultimately eliminate the difference between the tail and unperturbed LISM. We find that the mixing length becomes equal to the smallest heliosphere width of about 90 au at a distance of about 2,500 au. When this happens, the heliopause is completely destroyed. In the absence of locally generated turbulence, the mixing length becomes equal to the tail thickness at 8,000-20,000 au. The distance at which the effect of the heliosphere completely disappears and the properties of the pristine LISM are established may exceed 0.5 pc.