The excitation of helium resonance lines in solar flaresHelium resonance line intensities are calculated for a set of six flare models corresponding to two rates of heating and three widely varying incident fluxes of soft X-rays. The differing ionization and excitation equilibria produced by these models, the processes which dominate the various cases, and the predicted helium line spectra are examined. The line intensities and their ratios are compared with values derived from Skylab NRL spectroheliograms for a class M flare, thus determining which of these models most nearly represents the density vs temperature structure and soft X-ray flux in the flaring solar transition region, and the temperature and dominant mechanaism of formation of the helium line spectrum during a flare.
Document ID
19860057652
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Porter, J. G. (NASA Marshall Space Flight Center Huntsville, AL; Joint Institute for Laboratory Astrophysics, Boulder, CO, United States)
Gebbie, K. B. (Joint Institute for Laboratory Astrophysics Boulder, CO, United States)
November, L. J. (National Solar Observatory Sunspot, NM, United States)