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J. M. Laming (NRL)
The means and sensitivity with which the Sun is routinely observed have dramatically changed in the last decade, and will continue to do so into the next. I will discuss how this changes the atomic physics data required for analysis and interpretation of solar observations. In particular, the trend of spectroscopic instrumentation to the high throughput devices possible with multilayer optics, and the corresponding necessity of rather narrow spectral bandwidths make accurate ionization balance calculations, and correspondingly accurate rates to go into them, essential. The shorter exposure times afforded by multilayer optics bring observing departures from ionization equilibrium in coronal spectra closer to reality, again requiring accurate ionization recombination rates. Departures from ionization equilibrium are already observed in situ in various regions of the solar wind, and I will describe how one can use such information to make inferences on electron heating in the fast solar wind and the origin of plasma in coronal mass ejections. Work supported by NASA Contract S13783G and by the NRL/ONR Solar Magnetism and the Earth's Environment 6.1 Research Option.
The author(s) of this abstract have provided an email address for comments about the abstract: jlaming@ssd5.nrl.navy.mil
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Bulletin of the American Astronomical Society, 36 #2
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