Solar Physics Division Meeting 2000, June 19-22
Session 2. Corona, Solar Wind, Flares, CMEs, Solar-stellar, Instrumentation, Other
Display, Chair: J. Krall, Monday-Thursday, June 19, 2000, 8:00am-6:00pm, Forum Ballroom

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[2.100] Investigation of Chromospheric and Coronal Structures with the Advanced Technology Solar Spectroscopic Imager

P.F.X. Boerner (Stanford University Department of Physics), K. Wamba, D.S. Martinez-Galarce, A.B.C. Walker, B. Cabrera (Stanford University Department of Physics), L. Lesyna (Lockheed-Martin), K. Irwin, S.W. Nam, S. Deiker (National Institute of Standards and Technology, Boulder, CO), R.B. Hoover (Marshall Space Flight Center), T.W. Barbee (Lawrence Livermore National Laboratory)

We discuss a new rocket payload, the Advanced Technology Solar Spectroscopic Imager (ATSSI), that will obtain true spectroheliograms from ~ 300 Å\ to 1.5 Å. Using an array of quantum calorimeter detectors at the focus of a Wolter I telescope, it will obtain approximately 1000 spectra spanning the energy range from 150 eV to 3 keV with ~ 3 eV energy resolution and covering a 3.5 arc-minute by 3.5 arc-minute field of view with 6.25 arc-second pixels. Each spectrum will include spectral lines from ions ranging from C V to S XVI, generated over the temperature range from 600,000 K to > 10,000,000 K. The ATSSI will also obtain full-disk images in lines of Fe XVII, Fe XII, Mg X, Fe IX, Ne VIII, O VI, C IV, and H I, all with resolution of ~ 1-2 arc-seconds, and high-resolution grating spectroheliograms in lines of Fe IX/X, O V/VI, and Mg II. These observations can be used to (a) model the flow of energy in the small structures associated with the chromospheric network, and investigate the nature of their interface with transition region and coronal plasmas; and (b) observe the thermal structure of coronal loops in sufficient detail to determine the spatial distribution of their non-thermal heating mechanism(s).

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