<LI><A NAME="tex2html1" HREF="node3.html#30">Hubble GHRS spectrum of Capella [Linsky et al., 1992; Lallement, 1992]. </A>
<LI><A NAME="tex2html3" HREF="node4.html#68">Schematic of the plasma boundaries expected in the outer heliosphere. 
</A>
<LI><A NAME="tex2html4" HREF="node4.html#125">Simulation results of Zank et al. [1996] for the temperature (colour coding) and the plasma density 
relative to the VLISM plasma density (contours), with arrows showing the direction of the plasma flow. 
The heliopause (HP), termination shock (TS), and bow shock (BS) are clearly visible. </A>
<LI><A NAME="tex2html5" HREF="node4.html#129">Simulation results of Zank et al. [1996] for the plasma density as a 
function of heliocentric distance in the upwind (full line), transverse (dotted line), and 
downwind (dashed line) directions. 
directions.</A>
<LI><A NAME="tex2html6" HREF="node6.html#137">Dynamic spectrum of Voyager 1 data, showing the 1983-1984 and 1992-1993 outbursts of 
radiation from the outer heliosphere [Gurnett and Kurth, 1995]. The dark, very uniform band from 
 <IMG WIDTH=78 HEIGHT=20 ALIGN=MIDDLE ALT="tex2html_wrap_inline352" SRC="img1.gif"  >  kHz is interference from the spacecraft power supply. </A>
<LI><A NAME="tex2html7" HREF="node6.html#151">Cosmic ray counts from the Deep River Neutron Monitor are compared with the flux densities of 
the outer heliospheric radiation measured by Voyager 1 [Gurnett and Kurth, 1995]. </A>
<LI><A NAME="tex2html8" HREF="node6.html#155">Cosmic ray counts from the Deep River Neutron Monitor and the Pioneer and Voyager spacecraft are 
compared as functions of heliocentric distance and time for the disturbance that apparently triggered 
the 1992-1993 radio emissions [Gurnett et al., 1993]. </A>
<LI><A NAME="tex2html9" HREF="node6.html#230">Dynamic spectrum of  <IMG WIDTH=13 HEIGHT=23 ALIGN=MIDDLE ALT="tex2html_wrap_inline354" SRC="img2.gif"  >  and  <IMG WIDTH=21 HEIGHT=23 ALIGN=MIDDLE ALT="tex2html_wrap_inline356" SRC="img3.gif"  >  radiation generated upstream of a shock 
moving with constant isotropic speed through the 3-D plasma density structures shown in Figures 20.3 and 
20.4 [Cairns and Zank, 1999]. </A>
