Fiber fine structures superposed on the continuum emission of solar type IV burst

Details Fiber fine structures superposed on the continuum emission of solar type IV burst Fiber fine structures superposed on the continuum emission of solar type IV burst

Mar 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pbeio..38...72z&link_type=abstract

Astrophysics Reports. Publications of the Beijing Astronomical Observatory, No. 38, p. 72 - 77 (2002). In: Proceedings of the Ni

Astronomy and Astrophysics

Astrophysics

Solar Flare, Radio Burst, Fiber Structures

Scientific paper

On July 14, 2000, a type IV solar radio burst was observed at 10:43 - 11:00 UT with the 1 - 2 GHz digital spectrometer of National Astronomical Observatories of China (NAOC). Many fiber fine structures superposed on the type IV burst were detected in the same interval. The typical values of frequency drift for those fibers were in the range of -47.4 to -89.3 MHz s-1. A theoretical interpretation for the fibers is based upon the model of a magnetic-mirror loop configuration in the solar corona. In this model, the source of the fiber emission is considered as the ducting of whistler solitons within the magnetic mirror loop. After quantitatively estimating using the observed data, it is indicated that the magnetic field strength of the radio source is of about 145.1 ≤ B0 ≤ 273.4 gauss. It is also indicated that a fiber is composed of 4×1015 solitons occupying a volume of about 1.2×108 km3. For the duct through which the whistler solitons passed within the magnetic-mirror loop, we obtain the diameter of the duct to be of d ≍ 120 km and the length of the duct to be of Δr ≍ 104 km, respectively.

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