ИСТИНА

When the supersonic solar wind interacts with the interstellar medium, a gas-dynamic structure called the heliospheric shock layer is formed. This structure consists of a tangential discontinuity (known in astrophysics as the heliopause), a solar wind termination shock, and a bow shock in the interstellar medium. The distance to the heliospheric shock layer, as well as its thickness, are significantly influenced by magnetic fields (both heliospheric and interstellar) and by interstellar hydrogen atoms, which interact with the solar wind plasma and the interstellar medium via charge exchange. This paper investigates the effect of electron thermal conductivity, which is anisotropic and acts along the magnetic field lines. Particular attention is paid to the tail region of the interaction area. It is shown that accounting for thermal conductivity leads to a decrease in the thickness of the inner part of the shock layer between the termination shock and the tangential discontinuity. It was found that the effect of thermal conductivity significantly alters the plasma temperature and density values, which may be substantial for the analysis of Lyman-alpha absorption spectra in the directions