<LI><A NAME="tex2html1" HREF="node2.html#9">A dipole source of magnetic field is imposed at the 
photosphere and the MHD equations are used to construct the magnetic field lines 
in the cases with (solid lines) and without (dashed lines) a self-consistent 
solar wind outflow [Pneuman and Kopp, 1971]. </A>
<LI><A NAME="tex2html2" HREF="node2.html#13">An artist's sketch of the plasma structure and magnetic configuration 
expected near the solar equator [Hundhausen, 1972]. </A>
<LI><A NAME="tex2html3" HREF="node2.html#17">The ``ballerina skirt'' ripples predicted on the heliospheric current sheet 
[Dryer, 1998]. </A>
<LI><A NAME="tex2html4" HREF="node3.html#22">The time-averaged away/toward the Sun (positive/negative) components of the magnetic field in the 
solar wind (solid lines) are compared with the disk-averaged away/toward component of the 
photospheric magnetic field (dashed lines) [Severney et al., 1970]. </A>
<LI><A NAME="tex2html5" HREF="node3.html#26">Illustration of sectors of magnetic field lines with different polarities 
[Cravens, 1997]. </A>
<LI><A NAME="tex2html6" HREF="node3.html#30">The lefthand figures show contours of the X-ray brightness of the corona and 
the sense of the vertical component of the coronal magnetic field direction. The 
righthand figures show the solar wind speed and the polarity of the radial 
component of the solar wind magnetic field. Adapted from Hundhausen [1972]. </A>
<LI><A NAME="tex2html7" HREF="node3.html#34">Colour illustration of the solar wind speed and the sense of the magnetic 
field's radial component observed as a function of heliolatitude by the Ulysses 
spacecraft [McComas et al., 1998]. </A>
<LI><A NAME="tex2html8" HREF="node4.html#39">Schematic illustration of a fast stream interacting with a slow stream 
[Hundhausen, 1972].</A>
<LI><A NAME="tex2html9" HREF="node4.html#44">Superposed-epoch analysis of the plasma parameters for CIRs [Gosling et al., 
1996]. Note the well defined 
pressure pulse and compression region in the modified portion of the slow stream. </A>
<LI><A NAME="tex2html10" HREF="node4.html#59">Evolution towards a CIR state of a high temperature region imposed at the 
inner boundary of the 
solar wind [Hundhausen, 1973]. Note the development of shocks, a pressure pulse, and 
the characteristic two-step increase and decay of the solar wind speed. Yes there is one</A>
<LI><A NAME="tex2html11" HREF="node4.html#63">Figure from Smith [1985] described in the text.</A>
<LI><A NAME="tex2html12" HREF="node4.html#67">The top panel shows the plasma density profiles observed by IMP 7 near 1 AU and by 
Pioneer 10 near 4.5 AU. The bottom panel compares the measured Pioneer 10 density structure 
with that predicted by a 1-D MHD code using the IMP 7 data as input. Very good agreement 
is evident [Gosling et al., 1976].</A>
<LI><A NAME="tex2html13" HREF="node4.html#71">MHD simulation of (1) high speed streams which cause the development 
of CIR structure and (2) the propagation of transient shocks which also modify 
the CIR structure (bottom two panels particularly) [Akasofu and Hakamada, 1983]. </A>
<LI><A NAME="tex2html14" HREF="node5.html#76">Schematic of a coronal mass ejection in the form of a magnetic cloud [Cravens, 
1997] with a shock.</A>
<LI><A NAME="tex2html15" HREF="node5.html#80">Plasma parameters of a CME and associated shock observed near 1 AU [Gosling, 1996]. </A>
<LI><A NAME="tex2html16" HREF="node5.html#84">Example of a CME and associated forward/reverse shock pair observed by 
Ulysses near 5 AU [Gosling, 1996]. </A>
