Structure of impulsive phase of solar flares from microwave observations

Details Structure of impulsive phase of solar flares from microwave observations Structure of impulsive phase of solar flares from microwave observations

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981stin...8133112p&link_type=abstract

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Physics

Microwaves, Solar Electrons, Solar Flares, Solar X-Rays, Loops, Pitch (Inclination), Solar Magnetic Field, Solar Maximum Mission, Synchrotron Radiation, Very Large Array (Vla)

Scientific paper

Variation of the microwave intensity and spectrum due to gyro-synchrotron radiation from semi-relativistic particles injected at the top of a closed magnetic loop is described. Using the recent high spatial resolution X-ray observations from the HXIS experiment of Solar Maximum Mission and from observations by the Very Large Array (VLA), it is shown that the high microwave brightness observed at the top of the flare loop can come about if (1) the magnetic field from top to footpoints of the loop does not increase very rapidly, and (2) the accelerated particles injected in the loop have a nearly isotropic pitch angle distribution. The limits on the rate of increase of the magnetic field and/or the average pitch angle depend on the geometry and location of the loop on the solar disk.

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