The latitudinal structure of the heliospheric magnetic field during mu
ch of the solar cycle is determined by a ''sector zone'', in which bot
h positive and negative magnetic polarities are observed, and by the u
nipolar regions above and below the sector zone. Distinct corotating s
treams and interactions regions are found primarily in the sector zone
during the declining phase of the solar cycle. Within a few AU, the s
treams and interaction regions are distinct and are related to solar f
eatures. A restructuring of the solar wind occurs between 1 AU and app
roximate to 15 AU, in which the isolated streams, interaction regions
and shocks merge to form compound streams and merged interaction regio
ns (''MIRs''). Memory of the source conditions is lost in this process
. In the region between approximate to 30 AU and the termination shock
(the ''distant heliosphere''), the pressure of interstellar pickup pr
otons dominates that of the magnetic field and solar wind particles an
d largely controls the dynamical processes. During 1983 and 1994, coro
tating streams and corotating interaction regions were observed at 1 A
U. Merged interaction regions were observed at approximate to 15 AU in
1983, but not at approximate to 45 AU during 1994. This result sugges
ts a further restructuring of the solar wind in the distant heliospher
e, but variations from one solar cycle to the next might also contribu
te to the result. Approaching solar minimum in 1996, the latitudinal e
xtent of the sector zone decreased, and Voyager 2 gradually entered th
e unipolar region below it. The speed was lower in the sector zone tha
n below it. At Voyagers 1 and 2, the change in cosmic ray intensity is
related to the magnetic field strength during each year from 1983 thr
ough 1996. The magnetic field strength has a multifractal distribution
throughout the heliosphere. This fundamental symmetry of the heliosph
ere has not been incorporated explicitly in cosmic ray propagation mod
els.