Diagnostic Tools

1. Using HI 1216 Å profile measurements, determine observational constraints on the proton velocity distribution function (including constraints on the proton temperature and non-thermal velocity) in various coronal structures.
2. Using HI 1216 Å profile and visible light measurements, derive outflow velocities of protons in coronal streamers, coronal holes and the quiet sun (Doppler dimming).
3. Using OVI 1032 - 1037 Å , MgX 610 - 625 Å , and SiXII 499 - 521 Å intensity measurements (both resonantly scattered and collisionally excited components) together with visible light measurements, determine outflow velocity and abundance of , and coronal structures (Doppler dimming).
4. Using measurements of the electron-scattered HI 1216 Å profile, determine the electron temperature and density in various coronal structures.
5. Using ratio of resonantly-scattered HI 1216 Å intensity and visible light, determine an ionization temperature in a streamer and compare with temperature derived from line width of electron scattered HI 1216 Å.
6. Using solar disk measurements of HI 1216 Å, HI 1025 Å, OVI 1032 - 1037 Å, SiXII 499 - 521 Å, MgX 610 - 625 Å, FeXII 1242 Å profiles and intensities, and disk visible intensities, obtain intensity and line profile maps of the solar disk for analysis of coronal data.
7. Using line profiles of OVI 1032 - 1037 Å, Si XII 499 - 521 Å, MgX 610 - 625 Å, and FeXII 1242 Å, determine kinetic temperatures in various coronal structures.
8. Using resonantly-scattered HI 1025 Å to HI 1216 Å ratio and visible polarized radiance, determine an ionization temperature in various coronal structures, and compare with electron temperature derived from electron scattered HI 1216 Å.