Theoretical Ne v emission line ratios compared to solar observations
Abstract
The recent level population calculations for Ne v by Aggarwal are used to determine the theoretical emission line ratios R1 = I(2s2p31Do - 2s22p21De)/I(2s2p33D20- 2s22p23P1e) and R2 = I(2s2p31Do-2s22p21De)/I(2s2p33D30-2s22p23P2e). A comparison of these with observational data for a solar flare and erupting prominence obtained with the NRL XUV spectrograph on board Skylab reveals that R1 and R2 are in their predicted high density limits. Although the ratios cannot be used as density diagnostics for values of ne typical of the solar transition region, it is shown that they are temperature sensitive and hence may be employed to determine the electron temperatures of Ne v line emitting regions.
- Publication:
-
Solar Physics
- Pub Date:
- May 1986
- DOI:
- 10.1007/BF00156375
- Bibcode:
- 1986SoPh..105...47K
- Keywords:
-
- Emission Spectra;
- Line Spectra;
- Neon;
- Solar Spectra;
- Electron Orbitals;
- Solar Flares;
- Solar Prominences;
- Solar Physics;
- Flare;
- Observational Data;
- Level Population;
- Transition Region;
- Emission Line