What Solar Atmospheric Pnenomena Produce the Suns X-ray-EUV-UV Spectrum?
G. A. Doschek (E. O. Hulburt Center for Space Research, Naval Research Laboratory) Recently high-resolution X-ray-EUV-UV spectra of unprecedented spectral resolution have been obtained from non-solar cosmic sources from missions such as Chandra, EUVE, and HST. These spectra have resolving power that rivals the best solar spectra, and detailed plasma diagnostic techniques can be used to interpret them. Many of the plasma diagnostic techniques were first developed and used for the interpretation of high-resolution solar, tokamak, and laser-produced plasma spectra. However, detailed spatial resolution of at least stellar sources is still lacking. In this talk I will illustrate what regions and processes in the solar atmosphere produce different sections of the Sun’s high-energy spectrum. I will link various spectral features with the most recent high-resolution spatial observations of the Sun, and discuss the physical mechanisms that are believed to define the morphology and energetics of
