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Observations and analysis of solar flares using H. cap alpha. spectral profiles

Thesis/Dissertation ·
OSTI ID:6249397
This dissertation approaches the chromospheric flare problem in three steps: analysis of an observed flare using existing empirical models; development of new physical models of H..cap alpha..; and analysis of another observed flare using these physical models. First, the flare of 1980 May 7 is analyzed using H..cap alpha.. spectral profiles from Sacramento Peak Observatory and cotemporal X-ray observations from the Solar Maximum Mission spacecraft. Through comparison of the observed profiles with the empirical H..cap alpha.. profiles, it is shown that chromospheric evaporation takes place concurrently with enhancement of the overlying coronal density. During the impulsive phase, it is suggested that evaporation is driven by flare-accelerated electrons. During the thermal phase, it can only be driven by thermal conduction. Next, physical models of H..cap alpha.. spectral profiles are calculated for a grid of model flare chromospheres, in both the hydrostatic and impulsive approximation. It is shown that only high fluxes of nonthermal electrons produce broad, nonGaussian profile wings, and that only high values of the coronal pressure can remove the central reversal of the profiles. Enhanced thermal conduction alone cannot account for enhanced H..cap alpha.. emission. Finally, the flare of 1980 June 24 is analyzed, showing that nonthermal electrons were accelerated bidirectionally within coronal loops and injected into the chromosphere at the loop footprints.
Research Organization:
California Univ., San Diego (USA)
OSTI ID:
6249397
Country of Publication:
United States
Language:
English