Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...258..542m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 258, no. 2, p. 542-548.
Astronomy and Astrophysics
Astrophysics
19
Coronal Loops, Coulomb Collisions, Energetic Particles, High Energy Electrons, Magnetically Trapped Particles, Solar Atmosphere, Solar Flares, Kinetic Equations, Magnetic Field Configurations, Maxwell-Boltzmann Density Function, Solar Magnetic Field, Spatial Distribution
Scientific paper
The temporal and spatial evolution of a population of high-energy electrons in a flaring coronal loop is simulated by solving numerically the appropriate kinetic equation. Coulomb collisions, reverse currents, magnetic field convergence, and precipitation, are all taken into account. Two scenarios are investigated: (1) electrons initially having a single-temperature Maxwellian distribution throughout the loop, the acceleration process having ceased; and (2) electrons accelerated isotropically close to the loop apex, the acceleration process having a linear rise and decay time profile. The spatial distribution of hard X-ray emission is determined, and in case (1) it is found that emission from the chromosphere (i.e. the loop footpoints) generally exceeds that from the corona, even when the magnetic field is strongly converging. Reverse current ohmic losses in the corona tend to reduce the chromospheric X-ray flux, while the coronal X-ray flux is unaffected. In case (2), X-ray emission is concentrated in the corona to a greater extent than in case (1), the spatial distribution of emission again depending on the magnitude of the reverse current. In agreement with previous authors, we find a positive correlation between ohmic losses and the timescale over which electrons are accelerated. We conclude that hard X-ray observations are best explained by pulsed, isotropic acceleration of electrons near the apex of a loop with a strongly converging magnetic field.
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