Whistler ray tracing calculations in the solar corona

Details Whistler ray tracing calculations in the solar corona Whistler ray tracing calculations in the solar corona

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989kfnt....5...32m&link_type=abstract

Kinematika i Fizika Nebesnykh Tel (ISSN 0233-7665), vol. 5, Nov.-Dec. 1989, p. 32-43. In Russian.

Physics

10

Ray Tracing, Solar Corona, Type 4 Bursts, Wave Propagation, Whistlers, Electron Density (Concentration), Numerical Integration, Solar Magnetic Field, Two Dimensional Models

Scientific paper

Whistler rays in the solar corona are traced using numerical integration of the Haselgrove (1971) two-dimensional equations for the magnetosphere. It is shown that many magnetospheric-type whistlers are typical of the solar corona. The refractive index in the corona can be very large and group propagation times between consecutive reflections may reach several minutes. Whistlers in the corona may be channeled along density and magnetic field inhomogeneities with widths in the range between 1000 and 2000 km. It is found that upward duct whistler propagation generated in the foot of the magnetic trap is related to fiber bursts, while nonducted propagation generated at the top of the magnetic loop is related to the zebra-structure in the pulsating regime in the continuum emission of type IV bursts.

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