Local Interstellar Cloud as Birkeland current

[celeste]

https://upload.wikimedia.org/wikipedia/ ... arrows.jpg
If the "clouds" in this picture have magnetic fields as described in Donald Scott's filament model, what would you expect to see looking on a line of sight towards Alpha Centauri, for example? Looking radially across the filament (filaments?), we should see that ever spiraling magnetic field direction. In Don's model, it is only when we look down a sight line parallel to the filament axis, that we should see the same magnetic field direction on our line of sight. In other words,if we look down towards the stars in the direction of Ophiuchus , we should see a consistent magnetic field direction across our line of sight. Now read the 4th and 5th paragraphs of 7.1.3 here http://www.wesleyan.edu/planetary/pubs/3_Frisch.pdf
" Tinbergen (1982) detected a patch of very weak interstellar polarization, ∼0.02%, near the
Sun in the fourth galactic quadrant and at negative ecliptic latitudes (Frisch 2005). The location
of the patch coincides with the G cloud (Section 3). The closest polarized star is 36 Oph, which
is 10◦ from the heliosphere nose (Section 3.2). "
And
"Five of the Tinbergen stars form a polarization peak toward the heliosphere nose, which is
defined by a consistent polarization position angle."

[celeste]

Not to mention, in 5.2 of the same article,where they talk about ionization gradients "between the edge of the cloud,and its deepest parts", that is Marklund convection.
They don't call it that. They think the gradient is caused by ionizing radiation, and its ability to penetrate the cloud. They admit,however,(point 2,under future issues,near the end of the article),they don't have a source nailed down for said ionization.