<LI><A NAME="tex2html1" HREF="node2.html#21">Alfven waves in the solar wind [Belcher and Davis, 1971]. The top 
three panels each show a different orthogonal component of the solar wind magnetic 
field and the associated (fluid) velocity component of the plasma. The bottom 
panel displays the magnitudes of the total magnetic field and flow speed.</A>
<LI><A NAME="tex2html2" HREF="node2.html#34">Schematic illustration of the power spectrum of MHD turbulence in 
the solar wind [Goldstein et al., 1995].</A>
<LI><A NAME="tex2html3" HREF="node2.html#38">Typical spectrum of interplanetary magnetic field turbulence showing the 
inertial and dissipation ranges [Leamon et al., 1998].</A>
<LI><A NAME="tex2html4" HREF="node3.html#43">Energetic protons associated with two CIRs are shown for one-half of a solar rotation 
together with the associated profile of the magnetic field [Scholer et al., 1980; Smith, 1985]. 
The particle intensity shows maxima in the vicinity of the forward and reverse shocks with 
minima near the peak field strength in each interaction region. The accelerated particles 
extend both well upstream and downstream from the shocks. 
</A>
<LI><A NAME="tex2html5" HREF="node3.html#47">Voyager observations of cosmic rays at CIRs near 8 AU [Burlaga et al., 1984; 
Smith, 1985]. The middle panel shows the ratio of the observed magnetic field strength 
to that predicted for the Parker spiral model. The first two shocks are associated 
with increases in the cosmic ray flux but followed by Forbush decreases in the high 
field regions behind the shocks.</A>
<LI><A NAME="tex2html6" HREF="node3.html#207">Count rates for protons, alpha particles and ``medium mass'' nuclei near an 
almost perpendicular ( <IMG WIDTH=62 HEIGHT=24 ALIGN=MIDDLE ALT="tex2html_wrap_inline394" SRC="img1.gif"  >  degrees) 
transient interplanetary shock [Armstrong et al., 1985]. The peaking of the count rates 
near the shock is consistent with shock drift acceleration.
</A>
<LI><A NAME="tex2html7" HREF="node3.html#66">Measured distribution function of interplanetary protons in the solar wind 
frame behind a transient interplanetary shock [Gosling et al., 1981; Scholer, 1985]. 
The distribution 
is composed of a thermal core of solar wind protons plus superposed power law tails 
consistent with diffusive shock acceleration. 
</A>
<LI><A NAME="tex2html8" HREF="node3.html#70">Exponential increases in the count rate of energetic particles with decreasing distance 
to an interplanetary shock, qualitatively consistent with diffusive shock acceleration [Scholer 
et al., 1983]. </A>
<LI><A NAME="tex2html9" HREF="node5.html#78">The solar wind plasma density as a function of heliocentric distance <I>R</I> [Belcher et al., 
1993]. </A>
<LI><A NAME="tex2html10" HREF="node5.html#212">Voyager 1 observations of the magnetic field strength versus time (solid dots) and 
Parker's prediction (solid curve) taking into account variable solar wind speed and variable 
source fields in the photosphere [Burlaga et al., 1998]. The dotted curves show Parker's 
predictions for 
variable source fields but constant solar wind speeds of 800 and 400 km s <IMG WIDTH=14 HEIGHT=7 ALIGN=BOTTOM ALT="tex2html_wrap_inline402" SRC="img2.gif"  >  for the 
bottom and top curves, respectively. </A>
<LI><A NAME="tex2html11" HREF="node5.html#101">A cut through a  solar wind electron distribution along the magnetic field 
direction [Feldman, 1979]. The two solid curves are two bi-Maxwellian functions 
which best fit the core and halo electrons at low and intermediate energies, 
respectively. </A>
<LI><A NAME="tex2html12" HREF="node6.html#215">The top portion shows the pickup ring, solar wind flow, and the directions of the 
solar wind velocity, electric, and magnetic fields in the <B>solar</B> frame: pickup ions 
are born at zero velocity but are then sped up by the convetion electric field to develop 
a gyrospeed equal to  <IMG WIDTH=23 HEIGHT=14 ALIGN=MIDDLE ALT="tex2html_wrap_inline404" SRC="img3.gif"  > . The bottom portion is a contour plot of the ion velocity 
distribution in the solar wind frame, showing the solar wind protons near zero velocity 
and the pickup ions in a ring distribution. </A>
<LI><A NAME="tex2html13" HREF="node6.html#217">The phase space density of interstellar pickup protons as a function of  <IMG WIDTH=40 HEIGHT=24 ALIGN=MIDDLE ALT="tex2html_wrap_inline406" SRC="img4.gif"  >  
observed in the spacecraft frame by Ulysses at 4.2 AU [Gloeckler et al., 1993].
</A>
<LI><A NAME="tex2html14" HREF="node6.html#153">Proton temperature data observed by the Voyager 2 
spacecraft (jagged curve) are compared with the predictions of adiabatic 
cooling (dotted curve and a turbulent heating model including heating by CIRs alone (solid 
curve) and by pickup ions and CIR heating (dashed curve) [Williams et al., 1995]. 
</A>
<LI><A NAME="tex2html15" HREF="node6.html#157">The speed, density-weighted speed, and number flux for solar wind protons 
measured by the Voyager 2 spacecraft in the outer solar system (solid curve) and 
by the IMP 8 spacecraft at 1 AU (dotted curve) [Richardson et al., 1995]. Note that 
the solar wind speed 
is approximately constant with heliocentric distance but with the suggestion 
of a small decrease beyond about 15 AU.
</A>
<LI><A NAME="tex2html16" HREF="node7.html#162">Sample magnetic power spectrum measured by GIOTTO sunward of Comet Grigg-Skjellerup 
[Glassmeier and Neubauer, 1993]. 
The dashed line shows the cyclotron frequency for water ions. 
</A>
