<LI><A NAME="tex2html1" HREF="node2.html#25">Degradation of the solar cell array on a spacecraft with time due to damage by 
energetic particles [Goldhammer et al., 1976]. The step function decrease was due to the 
protons from one large solar flare. </A>
<LI><A NAME="tex2html2" HREF="node2.html#143">Currents induced in transformer windings of power stations in the northern USA 
(top), a magnetogram trace from Canada for the same period (middle),  and time variations 
in the index  <IMG WIDTH=24 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline330" SRC="img1.gif"  >  for the ring current associated with a substorm [Williams, 1979]. </A>
<LI><A NAME="tex2html3" HREF="node4.html#40">X-ray, energetic proton, and magnetic data from the GOES-7 spacecraft, the 
horizontal component of the magnetic field measured at Boulder, CO, USA, and the cosmic 
ray flux measured by the Deep River Neutron Monitor for the period 5 - 6 March, 
1989 [Allen et al., 1989].</A>
<LI><A NAME="tex2html4" HREF="node4.html#146">Solar wind monitor data ( <IMG WIDTH=23 HEIGHT=14 ALIGN=MIDDLE ALT="tex2html_wrap_inline332" SRC="img2.gif"  > ,  <IMG WIDTH=28 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline334" SRC="img3.gif"  > , and  <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  > ) and geomagnetic 
activity indices Kp and  <IMG WIDTH=24 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline330" SRC="img1.gif"  >  for the period 4 - 24 March 1989.</A>
<LI><A NAME="tex2html5" HREF="node4.html#55">Data for the period 13 -14 March 1989 in the same format as Figure 15.3 [Allen et 
al., 1989]. </A>
<LI><A NAME="tex2html6" HREF="node4.html#63">Count rates of energetic electrons versus time and energy from 
Los Alamos instruments on three geosynchronous spacecraft for 13 March, 1989. Note 
the strong injections near 2100 UT for two of the spacecraft. </A>
<LI><A NAME="tex2html7" HREF="node4.html#67">Southern hemisphere auroral images taken by the Dynamics Explorer 1 (DE-1) spacecraft 
Allen et al. [1989]. At left is a quiet time auroral ring (22 March, 1983) and at right 
is the largest auroral zone recorded by DE-1 up to 1826 UT on 13 March 1989.</A>
<LI><A NAME="tex2html8" HREF="node4.html#71">Solar wind data for the January 1997 storm period, as presented by L.F. Burlaga 
on the ISTP web site. The CME shock and cloud, plus a subsequent CIR, are clearly 
identified.</A>
<LI><A NAME="tex2html9" HREF="node4.html#152">Geomagnetic activity indices  <IMG WIDTH=56 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline340" SRC="img5.gif"  >  and  <IMG WIDTH=24 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline330" SRC="img1.gif"  >  for the period 
8 - 12 January 1997, obtained from the OmniWeb site.</A>
<LI><A NAME="tex2html10" HREF="node4.html#154">Ground-based and spacecraft data showing different aspects of geomagnetic activity 
for the January 1997 space weather events: (top) ground-based Canopus magnetometer data showing the 
magnetic perturbations of the auroral electrojets as a proxy for AE, (second) energetic 
electron fluxes measured at geosynchronous orbit, showing discrete injections on day 10 
and before as well as the increase in flux level due to enhanced solar fluxes, (third) 
ground-based SESAME magnetometer data, and (bottom) magnetometer data from the Wind spacecraft 
showing how these magnetospheric variations  are associated with southwards  <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  > </A>
<LI><A NAME="tex2html11" HREF="node4.html#94">Auroral displays on 10 January 1997; The top-left image shows a quiet auroral oval 
before the storm. The top-right and bottom-left images are during the height of the storm, 
showing the auriral oval to have expanded, broadened and brightened greatly. The final image 
shows how quickly the auroral displays can disappear.</A>
<LI><A NAME="tex2html12" HREF="node4.html#157">Dependence of the AL index for substorm magnetic activity on  <IMG WIDTH=23 HEIGHT=14 ALIGN=MIDDLE ALT="tex2html_wrap_inline332" SRC="img2.gif"  >  and 
 <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  >  [Muruyama et al., 1980; McPherron, 1995]. The abscissa is the value of AL normalized 
by  <IMG WIDTH=23 HEIGHT=27 ALIGN=MIDDLE ALT="tex2html_wrap_inline350" SRC="img6.gif"  > , while the ordinate is either the hourly average of  <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  >  when  <IMG WIDTH=48 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline354" SRC="img7.gif"  >  
or else a duration-weighted value of  <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  >  called  <IMG WIDTH=17 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline358" SRC="img8.gif"  >  for  <IMG WIDTH=48 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline360" SRC="img9.gif"  > . Statistically, substorm 
activity is clearly associated with long duration and/or large values of southward  <IMG WIDTH=18 HEIGHT=22 ALIGN=MIDDLE ALT="tex2html_wrap_inline336" SRC="img4.gif"  > .</A>
<LI><A NAME="tex2html13" HREF="node5.html#159">Magnetic topologies and  <IMG WIDTH=45 HEIGHT=20 ALIGN=MIDDLE ALT="tex2html_wrap_inline364" SRC="img10.gif"  >  convection velocities for Earth's 
magnetosphere under northwards and southwards solar wind magnetic field conditions. 
Dashed lines show the locations of the bow shock and magnetopause. Solid lines show 
illustrative magnetic field lines in the solar wind, magnetosheath, and magnetosphere either 
before or well after reconnection. Dotted lines show magnetic field lines fairly soon 
after reconnection.</A>
<LI><A NAME="tex2html14" HREF="node5.html#122">Definitions of the main phases of a magnetic substorm in terms of two 
auroral activity indices AU and AL [McPherron, 1995].</A>
<LI><A NAME="tex2html15" HREF="node5.html#126">The main stages in the ejection of a plasmoid during a magnetic substorm. 
[Hones, 1984; Cravens, 1997].</A>
