The table below summarizes the variations in FUV brightness observed during the flare.
 

Summary Bullets:
 

• Greatest variation in dayglow brightness are seen in emissions driven by photoelecton excitation, N2-LBH and OI-135.6.

• The smallest variation (10%) is observed in the direct resonantly-scattered HI emissions observed in GEO Tube 2.

• The variation in the S12 channel is much greater than the variation one would expect if the emission were due to 'leakage' of Lyman-Alpha. It is most certainly due to variability in the NI-120.0 emission.

• The smaller variation is seen in NI-120.0 emission may reflect the fact that the source is due to dissociative excitation of N2, which can branch to other states.

Future work - Possible IMAGE Collaborations

Comparisons with IMAGE EUV brightness variations for indirect measurement of solar EUV variation (which contributes to photoelectron production)

Further characterization of airglow variations vs. Dst for possible detection of ENA precipitation (Stephan et al, GRL, 2865, September 2000)

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