Gladstone, G. R., R. Link, G. Crowley, S. C. Solomon, and P. H. Reiff, Simulation IMAGE Far-Ultraviolet Auroral Observations presented at the American Geophysical Union Fall Meeting, San Francisco, December 15-19, 1996. Simulation IMAGE Far-Ultraviolet Auroral Observations G. R. Gladstone; R. Link; G. Crowley (all at: Southwest Research Institute, 6220 Culebra Road, San Antonio, TX 78238; ph. 201-522-3581; e-mail: randy@shistler.space.swri.edu); S. C. Solomon (LASP, University of Colorado, Boulder, CO 80303; ph. 303-492-6423; e-mail: solomon@tethys.colorado.edu); P. H. Reiff (Dept. of Space Physics, Rice University, Houston, TX 77251; ph. 713-527-4634; e-mail: reiff@alfven.rice.edu) We present several "realistic" simulated images of the far-ultraviolet auroral emissions of HI 1216Å (proton generated) and OI 1304Å (electron generated), as might be observed by instruments on the upcoming IMAGE spacecraft. Using estimates of precipitating particle fluxes and energies generated by the Rice Magnetospheric Specification and Forecast Model and the Hardy statistical model (J. Geophys. Res., 90, 4229, 1985; J. Geophys. Res., 94, 370, 1989) we follow ion and electron deposition at different locations (using the /glow transport code and realistic model atmospheres) to produce initial excitation rates for the 1216Å and 1304Å features. These excitation rates, along with the rates for background airglow emissions, are then corrected for radiative transfer effects (where needed), and the final excitation rates at many positions over the Earth are used to simulate images that would be seen by the Spectrographic Imager and Wideband Imaging Camera instruments on IMAGE. Several simulated images will be presented to show the evolution of the auroral oval during the magnetic cloud event of October, 1995.