Whistlers in the solar corona and their relevance to fine structures of type IV radio emission

Details Whistlers in the solar corona and their relevance to fine structures of type IV radio emission Whistlers in the solar corona and their relevance to fine structures of type IV radio emission

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..130...75c&link_type=abstract

(Committee of European Radio Astronomers, SNSF, URSI, et al., Workshop on Particle Beams in the Solar Atmosphere, Braunwald, Swi

Physics

29

Fine Structure, Solar Corona, Type 4 Bursts, Wave Propagation, Whistlers, Electron Diffusion, Magnetic Field Configurations, Magnetic Field Reconnection, Magnetohydrodynamic Stability, Ray Tracing, Solar Magnetic Field

Scientific paper

This short report concerns a general consideration of whistler manifestations in fine structures, including possible trajectories of obliquely propagating whistlers, the role of quasi-linear diffusion and an interpretation of new observations. A whistler ray tracing and kinetic whistler growth rates under arbitrary angles to the magnetic field in the solar corona were calculated. Different regimes of a whistler instability yield divers elements of fine structures: different stripes in emission and absorption or millisecond pulsations, moreover, zebra-stripes can convert into fiber bursts and inversely. A new explanation of low-frequency absorption in fibers is proposed: it is connected with an attenuation of plasma-wave instability due to the fast electron diffusion by whistlers. Role-like chains of fiber bursts are explained by a periodic whistler instability in a magnetic reconnection region.

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