  We know that it is the front of the bow shock where the solar wind kinetic
energy flux is transformed into the other kinds the most intensively. In our
previous studies, we obtained important relationships that enable calculating
the key parameters at transition through the bow shock front. One of the most
important sources of information on physical processes at the heliosphere
boundary are the Voyager 1 and 2 spacecrafts. Since both the solar wind and
interstellar medium are supersonic streams, two shocks are formed when flowing
around the heliopause. The internal shock, in which the solar wind decelerates
to subsonic velocity, is called the heliospheric shock. In the external bow
shock, the interstellar gas supersonic flux is decelerated. The aim of this
paper is to generalize the previously obtained equations to the processes in
the external bow shock region. If Voyager-1 was equipped with a greater set of
measuring instruments, we could have already provided estimations of the
interstellar medium key parameters, and described in physical terms what this
medium is, using relationships and equations from our studies.
