Hi Ben,
   Here are Wenbin's notes on the plots that he produced. These postscript
files can be found in the directory that we discussed.
   Ring me if there are any problems.
    Alan


The upper panels in figures 2-5 are the TING Model coarse grid 
(5x5 resolution) results, while lower panels are the TING Model 
fine grid (5/3x5/3)results.

Figure 1	Polar VIS Earth camera image at 18:59:44UT.
		This image was used as an input to the TING 
		Model to specify the energy flux, mean energy
		and auroral geometry.

Figure 2	The TING Model output of electron density at
		pressure level -4 and 19:00:00UT using POLAR VIS
		image (Figure 1) as auroral input. The TING Model was able 
		to simulate the fine structures seen in the POLAR image.

	The geophysical conditions for this simulation was that
	Kp = 3., CP = 60, and HP = 11, immediately after the Jan. 
	9th - 10th 1997 major geomagnetic storm.


Figure 3	Percentage changes of N2/O ratio under geomagnetic
		storm conditions calculated relative to geomagnetic 
		quiet conditions at 04:00:00UT. 
		The formula used to produce this plot was
		[(N2/O)storm-(N2/O)quiet]/(N2/O)quiet
		This silumation was done in April 9th-11th, 1997 UARC
		campaign. The quiet time was 04/09/97, the storm time
		was 11/04/87. A major geomagnetic storm occurred
		on 10-11/04/97 following a CME event.

Figure 4	The same as Figure 3, but for neutral temperature.
		Neutral winds (at 04:00:00UT of 11/04/97) were also
		plotted.	 

	Geophysical conditions for 04:00:00UT of 09/04/97 were
	Kp=2, CP=48, and HP=6. Both IMF data form WIND and Kp index
	were used in this simulation.
	The geophysiccal conditions for 04:00:00UT of 11/04/97 were
	Kp=6, CP=130, and HP=130. Both IMF data from WIND and the Kp 
	indices were used in this simulation.

Figure 5	A TING Model simulation for solar maximum, winter and
		quiet geomagnetic conditions (CP=60, HP=11). A tongue
		of ionization is seen to cross the polar cap in the fine
		grid results. A mid-latitude electron density trough 
		is also simulated.