The basic results of white-light flare (WLF) photometric and spectrographic observations are reviewed. WLFs represent the most extreme density conditions in solar optical flares and arc similar to stellar flares in many respects. It is shown that WLFs originate in the low chromosphere and upper phot
Electron beam as origin of white-light solar flares
โ Scribed by J. Aboudarham; J. C. Henoux
- Publisher
- Springer
- Year
- 1989
- Tongue
- English
- Weight
- 509 KB
- Volume
- 121
- Category
- Article
- ISSN
- 0038-0938
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โฆ Synopsis
We study the effect of chromospheric bombardment by an electron beam during solar flares. Using a semi-empirical flare model, we investigate energy balance at temperature minimum level and in the upper photosphere. We show that non-thermal hydrogen ionization (i.e., due to the electrons of the beam) leads to an increase of chromospheric hydrogen continuum emission, H -population, and absorption of photospheric and chromospheric continuum radiation. So, the upper photosphere is radiatively heated by chromospheric continuum radiation produced by the beam. The effect of hydrogen iomzation is an enhanced white-light emission both at chromospheric and photospheric level, due to Paschen and H-continua emission, respectively. We then obtain white-light contrasts compatible with observations, obviously showmg the link between white-light flares and atmospheric bombardment by electron beams.
๐ SIMILAR VOLUMES
A white-light flare (WLF) was recorded on March 27, 1991 at Tashkent. The WLF occurred at the penumbra of a large, complex sunspot group. The energy released by the WLF per unit time was 2.4 โข 10 ~ erg s -~ .
Electron bombardment of the solar atmosphere has two effects: one is to enhance hydrogen recombination emission, the other is to increase the opacity via an increase of H population. The first effect is the most important in the upper part of the atmosphere and the second in the lower part. We predi
The conditions required for the stability of a steady-state electron beam propagating in the solar corona are determined using the quasi-linear theory. The growth rate for electron plasma waves in a magnetized plasma is evaluated, with the electron distribution function being given by an analytic so