The Solar Upper Transition Region. I. High Resolution FUV-EUV Imaging and Modeling of Unresolved Coronal Funnels as Observed with the Multi-Spectral Solar Telescope Array, II

Details The Solar Upper Transition Region. I. High Resolution FUV-EUV Imaging and Modeling of Unresolved Coronal Funnels as Observed with the Multi-Spectral Solar Telescope Array, II The Solar Upper Transition Region. I. High Resolution FUV-EUV Imaging and Modeling of Unresolved Coronal Funnels as Observed with the Multi-Spectral Solar Telescope Array, II

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0206m&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.06; Bulletin of the American Astronomical Society, Vol. 32, p.811

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A coronal funnel model is tested against 171 Angstroms spectroheliograms recorded using a sounding rocket experiment flown on 3 November, 1994, called the Multi-Spectral Solar Telescope Array, II (MSSTA II). MSSTA, a joint project of Stanford University, the NASA Marshall Space Flight Center, and the Lawrence Livermore National Laboratory, is an observing platform composed of a set of normal-incidence, multilayer-coated optics designed to obtain narrow bandpass images at selected FUV, EUV and XUV wavelengths (44 Angstroms - 1550 Angstroms). Using the 1550 Angstroms (C IV) and 171 Angstroms (Fe IX/X) images, the funnel model, that is based on coronal back-heating, was constructed and tested against the data. Incorporating global coverage observations, we demonstrate that certain classes of funnels can account for the quiescent, globally diffuse and unresolved emission seen in 171 Angstroms spectroheliograms, suggesting this emission is mostly of upper transition region origin and composed mostly of Fe IX emission, as seen in the MSSTA observations. Furthermore, the classes of funnel models obtained, simultaneously satisfy areal coverage constraints observed at both 171 (60 - 90 confirmed by other solar observations.

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