**1. Introduction**

The medium we refer is evaluated to have a mixture of neutral 90% and plasma 10% with a particle density of about one particle (atoms + ions) per cm<sup>3</sup> . This value indicates a dilute electron density of 0.1 per cm3 . Also, the dominant feature Is the strong presence of a steady magnetic field (**B**-field) with a value that varies from about 0.4 to 0.7 nT. This medium has been in astrophysics already monitored remotely well before the arrival of the spacecraft (SC) Voyager 1 and 2 by the observation of 21 cm frequency signal provided by the e-flip in the orientation of its spin. These remote measurements have a localization uncertainty of 200 astronomic units (AUs), to which the Voyager SC brings a far better knowledge on the strong **B-**field localization through its in situ measurement. (Stone [1], announces that

Voyager 1 entered local interstellar medium (LISM)). The AU is defined by the mean distance of the Earth to the Sun which is equivalent to 150 solar radii (1 solar radius is the distance from the star center to its photosphere and is well-known to be 700,000 km with an uncertainty of possibly 0.1%). The in situ observations are achieved using in SC located magnetic field, radio, energetic particles, plasma instruments, respectively described respectively in [2–6].

In this work, we use both in situ observation by the SC (Sections 2, 3.1, 3.2, and by its combination with studies also performed by the author in similar strong magnetized MHD matter in Sections 3.3 and 3.4). Further, in Section 4, the author extrapolates the findings to astrophysical conditions from the realm solely of remote sensing (e.g. the Hubble telescope, and other more recent similar missions). Conclusions are drawn in Section 5.
