Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

Details Thermal cyclotron radiation from a hot coronal loop with helical magnetic field Thermal cyclotron radiation from a hot coronal loop with helical magnetic field

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ssrv...68..225s&link_type=abstract

Space Science Reviews, Volume 68, Issue 1-4, pp. 225-231

Statistics

Computation

5

Cyclotron Radiation, Solar Coronal Loop, Helical Magnetic Field, Gyroresonance Layer

Scientific paper

The spectral and polarization properties of thermal cyclotron radio emission from a hot coronal loop with a current along the axis are computed. The magnetic field is supposed to have a component along the loop axis as well as a poloidal part due to the current, both components being of comparable magnitude. In this specific configuration a helical magnetic field is present with a remarkable minimum of its absolute value along the loop axis and a maximum at its periphery. The presence of one or two maxima of magnetic field value along the line of sight results in increasing optical thickness of the gyroresonance layers at appropriate frequencies in the microwave band and, therefore, in enhanced radio emission at those harmonics which are optically thin (for example,s=4). These cannot be observed in models with the commonly employed magnetic field configuration (longitudinal along the loop axis). We show that the frequency spectrum of thermal cyclotron radiation from a hot coronal loop with a helical magnetic field differs from that of the standards-component source (with smooth frequency characteristics and polarization corresponding toe-mode) in that plenty of fine structures (line-like features and cut-offs) are present and theo-mode is prevalent in some frequency intervals. The enhanced radio emission at high harmonics and the complicated form of frequency spectrum in the model considered imply that some microwave sources, which are poorly explained in traditional models of solar active regions, may be associated with helical magnetic fields in hot coronal loops. Computations allow one to indicate spectral and polarizational peculiarities of local sources testifying to the presence of a helical magnetic field.

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