The Extreme Ultraviolet Imaging Spectrometer (EIS) on Solar-B

Details The Extreme Ultraviolet Imaging Spectrometer (EIS) on Solar-B The Extreme Ultraviolet Imaging Spectrometer (EIS) on Solar-B

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.3604d&link_type=abstract

American Astronomical Society, SPD meeting #37, #36.04; Bulletin of the American Astronomical Society, Vol. 38, p.260

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The Extreme Ultraviolet Imaging Spectrometer (EIS) for Solar-B is a high throughput state-of-the-art instrument designed to obtain solar spectra and images in two wavelength bands centered near 195 and 270 Angstroms. Traditional spectra can be obtained using narrow slits or images of solar structures can be obtained in individual spectral lines using wide slots. Essentially, the instrument obtains images in wavebands similar to TRACE but in each spectral line within the waveband. This removes electron temperature ambiguities inherent in broadband imagers and allows dynamic effects to be detected via Doppler shifts and densities and other plasma parameters to be measured via spectroscopic plasma diagnostics. After a brief description of how the instrument works and a comparison with previous instrumentation (sensitivity, etc.), the presentation will focus on the science that can be accomplished with EIS, presented in the form of sample observing sequences. The focus will be on active regions and solar flares with a consideration of topics such as temperature and density distributions in active region loops and their evolution, dynamical motions in active region loops, the reconnection site in solar flares, and temperature evolution of multimillion degree flare loops.

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