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Variable emission mechanism of a Type IV radio burst | | D. E. Morosan
; E. K. J. Kilpua
; E. P. Carley
; C. Monstein
; | | Date: |
4 Feb 2019 | | Abstract: | Context. The Sun is an active star and the source of the largest explosions
in the solar system, such as flares and coronal mass ejections (CMEs). Flares
and CMEs are powerful particle accelerators that can generate radio emission
through various emission mechanisms. Aims. CMEs are often accompanied by Type
IV radio bursts that are observed as continuum emission in dynamic spectra at
decimetric and metric wavelengths, but their emission mechanism can vary from
event to event. Here, we aim to determine the emission mechanism of a complex
Type IV burst that accompanied the flare and CME on 22 September 2011. Methods.
We used radio imaging from the Nanc{c}ay Radioheliograph, spectroscopic data
from the e-Callisto network, ARTEMIS, Ondrejov, and Phoenix3 spectrometers
combined with extreme-ultraviolet observations from NASA’s Solar Dynamic
Observatory to analyse the Type IV radio burst and determine its emission
mechanism. Results. We show that the emission mechanism of the Type IV radio
burst changes over time. We identified two components in the Type IV radio
burst: an earlier stationary Type IV showing gyro-synchrotron behaviour, and a
later moving Type IV burst covering the same frequency band. This second
component has a coherent emission mechanism. Fundamental plasma emission and
the electroncyclotron maser emission are further investigated as possible
emission mechanisms for the generation of the moving Type IV burst.
Conclusions. Type IV bursts are therefore complex radio bursts, where multiple
emission mechanisms can contribute to the generation of the wide-band continuum
observed in dynamic spectra. Imaging spectroscopy over a wide frequency band is
necessary to determine the emission mechanisms of Type IV bursts that are
observed in dynamic spectra. | | Source: | arXiv, 1902.1140 | | Services: | Forum | Review | PDF | Favorites | |
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