AAS 200th meeting, Albuquerque, NM, June 2002
Session 52. The Future of Extreme Ultraviolet Astronomy
Topical Session Oral, Wednesday, June 5, 2002, 8:30-10:00am, 10:45am-12:30pm, 2:30-4:00pm, 4:15-6:00pm, Morning in Ballroom A, Afternoon in Ballroom B

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[52.05] What Solar Atmospheric Pnenomena Produce the Sun's 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 the structures that produce the spectra. I will also discuss new spectral and atomic physics results that are emerging from the analysis of spectra from the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) spectrometer on the Solar and Heliospheric Observatory (SOHO) spacecraft. This work was funded by NASA Solar Physics Guest Investigator Grant S137816.

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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.