AAS 204th Meeting, June 2004
Session 29 The Solar Corona and Beyond
SPD Oral, Monday, May 31, 2004, 2:00-3:30pm, 702

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[29.02] Coronal Diagnostics based on EUV images from the Multi-Spectral Solar Telescope Array

P. Boerner (Stanford University)

The Multi-Spectral Solar Telescope Array flew from White Sands Missile Range on April 30, 2002, carrying 11 narrowband telescopes with bandpasses centered on emission lines ranging from 58 to 1550 Angstroms (covering the solar atmosphere from the temperature minimum to 2,000,000 K). The instruments were calibrated prior to flight, allowing the resulting images to be used for quantitative analysis of the temperature and density of the emitting plasma. Despite failures of some telescopes, spectroheliograms were obtained in 5 extreme ultraviolet bandpasses (centered on 150, 171, 180, 195 and 211 Angstroms) and 2 far ultraviolet bandpasses (centered at 1216 and 1550 Angstroms). These images, along with observations from EIT, can be used to constrain the differential emission measure of the corona in the temperature range of 800,000 to 2,000,000 K. I will present spatially-resolved differential emission measure functions obtained from the MSSTA data, and discuss the potential applications of these results along with the limitations of the current data set and of the DEM reconstruction technique.

The author(s) of this abstract have provided an email address for comments about the abstract: pboerner@stanford.edu

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