Multiple-wavelength analysis of energy release during a solar flare - Thermal and nonthermal electron populations

Details Multiple-wavelength analysis of energy release during a solar flare - Thermal and nonthermal electron populations Multiple-wavelength analysis of energy release during a solar flare - Thermal and nonthermal electron populations

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...357..662w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 357, July 10, 1990, p. 662-671.

Astronomy and Astrophysics

Astrophysics

18

Electron Density (Concentration), Energy Sources, Nonthermal Radiation, Solar Electrons, Solar Flares, Thermal Radiation, High Temperature Plasmas, Solar Corona, Solar Radio Emission, Very Large Array (Vla)

Scientific paper

Collaborative solar investigations by Tufts University and the Observatoire de Paris have resulted in simultaneous radio observations with the Very Large Array (VLA) and the Nancay Radioheliograph (NR), comparisons of this radio data with X-ray observations, and theoretical interpretations of the dominant radiation mechanisms during a weak impulsive solar flare observed on May 28, 1988. The VLA has mapped the flaring structures at time intervals of 3.3 s, showing that the preflash and flash-phase components of the impulsive emission originate in spatially separated sources. The 20.7 cm preflash source is ascribed to thermal gyroresonance emission from coronal loops with typical magnetic field strengths of up to 270 G; this emission is associated with heating and exhibits no detectable hard X-ray radiation above 30 keV. The flash-phase 20.7 cm source and the hard X-ray emission are attributed to nonthermal electrons in the coronal and chromospheric portions of a magnetic loop. The combination of imaging observations at 20.7 and 91.6 cm excludes emission from a confined hot plasma during the flash phase.

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