The Full Sun XUV Spectroscopy Imaging Instrument (SPIRIT) onboard CORONAS-F uses X-ray and extreme UV imaging spectroscopy to study the dynamics of active Sun from high resolution X and XUV spectral images in the 1,85-304 Å band; the dynamics of non-stationary solar events - flares, jets, CME in time scale from ~1 sec to months; the fine structure of solar plasma in flares, active regions, coronal holes with T = 0,05-50 MK; and the Fe- and He-ions distribution in solar disk and corona up to 5 solar radii . The SIPIRT is comprised of two components: the Solar X-Ray Telescope (SRT) and the X-Ray Spectroheliograph (RES-K).

The SRT, measuring the spatial structure and dynamics of the upper solar atmosphere, includes three optical channels: VR1, VR2 and SP (VR - "High Resolution", SP - "Wide Angle”). The High Resolution Channel VR1 has a Ritchey-Chretien lense (France), 1024x1152 CCD matrix, spectrum bands: 171Å (FeIX-FeXI), 195 Å (FeXII), 284Å (FeXV), 304Å (HeII) , 42' x 42' view angle(full disk) with angular resolution 1".4 - 2".5/cell and exposition time 0.5 - 100 sec. The High Resolution Channel VR2 has two paraboloids, 1024x1152 CCD matrix, spectrum bands: 175Å and 304Å with angular resolution up to 1".8/cell, view angle 30' x 30' and exposition time 0.04 - 100 sec. The Wide Angle Channel SP has a Ritchey-Chretien lense, 1024x1152 CCD matrix, spectrum band: 304Å with angular resolution 8"/cell, view angle 2° x 2° (up to 3 RO).

The RES-K instrument is an X-ray spectroheliograph to provide high-resolution images of the solar disk using the emission lines of FeXXIV and FeXXV in the 18.5-18.7 nm, and the MgXII line in the 84.1-84.3 nm range. Images in the emission lines covering 1800-2050 nm and 2850-3350 nm will also be obtained by scanning the range in widths of 0.3 nm. The images will be at a spatial resolution of six arc-sec. Each full-disk image is to be produced in about six seconds.