Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..431a&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 431-436. Research supported by SERC.
Astronomy and Astrophysics
Astrophysics
13
Emission Spectra, Radiation Trapping, Solar Corona, Solar Flares, X Ray Spectra, Electron Precipitation, Energetic Particles, Line Spectra, Magnetically Trapped Particles, Solar Magnetic Field
Scientific paper
Recent investigations into the impulsive phase of solar flares have led to the conclusion that the purely 'thick-target' models of flare X-ray emission are inconsistent with many observations. An alternative and possibly more realistic scenario is that of the trap-plus-precipitation model in which most of the hard X-ray emission emanates from the corona and is due to the bremsstrahlung of energetic electrons confined there by a converging magnetic field. In this model, the footpoint emission is caused by the precipitation of electrons out of the trap, via collisions, wave-particle interactions, or some other scattering process, into the high density chromospheric region of the flaring loop. The mean-scattering treatment of Coulomb collisional precipitation is discussed and the work of MacKinnon (1988) is extended to include electrons which are injected isotropically in pitch angle theta. These mean scattering results are compared with the Fokker-Planck calculations of McClements (1990), and it is shown that, for the isotropic injection case at least, the inclusion of dispersion in the electron distribution makes very little difference for the steady-state precipitated flux, for loss cone angles not smaller than 25 deg, corresponding to physically reasonable magnetic field ratios, Bchrom/Bcor not greater than 6. It is found that the total hard X-ray bremsstrahlung emission from such a coronal trap model can be consistent with observations of soft X-rays and the theoretically produced soft X-ray line profiles of Li et al. (1989).
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