Electron trapping in evolving coronal structures during a large gradual hard X-ray/radio burst

Details Electron trapping in evolving coronal structures during a large gradual hard X-ray/radio burst Electron trapping in evolving coronal structures during a large gradual hard X-ray/radio burst

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..149..171b&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 149, no. 1, p. 171-193

Physics

22

Evolution (Development), Magnetically Trapped Particles, Microwaves, Solar Corona, Solar Magnetic Field, Solar Radio Bursts, Solar X-Rays, Stellar Models, Coulomb Collisions, Deceleration, Electron Acceleration, Imagery, Light Curve, Magnetic Field Configurations, Mathematical Models

Scientific paper

Gradual hard X-ray/radio bursts are characterized by their long duration, smooth time profile, time delays between peaks at different hard X-ray energies and microwaves, and radiation from extended sources in the low and middle corona. Their characteristic properties have been ascribed to the dynamic evolution of the accelerated electrons in coronal magnetic traps or to the separate acceleration of high-energy electrons in a 'second step' process. The information available so far was drawn from quality considerations of time profiles or even only from the common occurrence of emissions in different spectral ranges. This paper presents model computations of the temporal evolution of hard X-ray and microwave spectra, together with a qualitative discussion of radio lightcurves over a wide spectral range, and metric imaging observations. The basis hypothesis investigated is that the peculiar 'gradual' features can be related to the dynamical evolution of electrons injected over an extended time interval in a coronal trap, with electrons up to relativistic energies being injected simultaneously. The analyzed event (26 April. 1981) is particularly challenging to this hypothesis because of the long time delays between peaks at different X-ray energies and microwave frequencies. The observations are shown to be consistent with the hypothesis, provided that the electrons lose their energy by Coulomb collisions and possibly betatron deceleration. The access of the electrons to different coronal structures varies in the course of the event. The evolution and likely destabilization of part of the coronal plasma-magnetic field configuration is of crucial influence in determining the access to these structures and possibly the dynamical evolution of the trapped electrons through betatron deceleration in the late phase of the event.

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