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An Eruptive Hot-Channel Structure Observed at Metric Wavelength as a Moving Type-IV Solar Radio Burst

V. Vasanth, Y. Chen, S. W. Feng, S. Ma, G. Du, H. Q. Song, X. L. Kong, and B. Wang


The sudden enhancements of non-thermal radio emission from the solar corona due to energetic electrons are observed as solar radio bursts. They  follow the solar activities such as flares and CMEs. It is well known  that there exist five types of radio bursts at the metric wavelength,  including type-I, II, III, IV and V. The type-IV radio bursts are  broadband continuum emission, further classified into moving and static  bursts. They are believed to be excited by energetic electrons within  certain magnetic structures such as magnetic arches, loops or plasmoids. Different emitting mechanisms have been proposed, including  gyro-synchrotron, plasma emission and electron cyclotron maser emission.

 

In recent years the SDO observations show that Hot Channel (HC) structures as one candidate of coronal flux ropes that are main energy carrier of  solar eruptions. The energetic electrons if existing within this HC-flux rope structure, can act as a possible source for emitting solar radio  bursts. This observation of a radio HC may provide a novel diagnostic  method to infer the properties of this critical structure.

 

Here we present the first radio imaging study of an eruptive HC structure in the metric wavelength. The associated radio emission observed on 4th March 2012 is manifested as a moving type-IV radio burst. The eruptive  structure is shown to be an HC structure, since it appears only in the  94 and 131 Å of SDO/AIA pass bands.

 

Figure 1 shows the observed eruptive HC structure in 94, 131 and 171 Å during  pre-eruptive, eruptive and post-eruption stages. The pre-eruptive stage  (top panels) shows the slow rise of flux rope structure from the active  region visible in 131 and 94 Å and not visible at 171 Å. The eruptive  stage (middle panels) shows the evolved plasmoid structure connected to a co-moving faint arcade feature, it is clearly observed at 131 Å. It  indicates that the structure contains high temperature plasmas. During  the eruption, the HC gradually fade and becomes invisible around 10:45  UT, while at its northwestern foot there appears an obvious dimming  region. The dimming is likely due to evacuation of plasmas (bottom  panels).



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Fig. 1 - The HC eruption recorded by AIA at 131, 94, and 171 Å at (a) 10:33  UT (to show the slowly rising HC, red arrows), (b) 10:40 UT (to show the eruptive plasmoid-HC structure, white arrows), and (c) 10:46 UT (to  show the dimming foot region, green arrows). S1 is for the distance  maps.

 

The moving type-IV (t-IVm) burst in the present study is recorded by  Artemis radio spectrograph and imaged by Nancy radio heliograph (NRH).  From Figure 2, we see a wide-band continuum emission from ~ 200 – 20 MHz with a trend of downward drift in time. The high frequency counterpart  is not clear possibly due to low sensitivity of the Artemis instrument  as well as the strong radio interference. Yet, according to the much  more sensitive measurements of NRH, there exist weaker yet significant  emissions from 150 – 445 MHz. Their corresponding flux, polarization and spectral index are shown in Figure2.



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Fig. 2 - Characteristics of the t-IVm burst as recorded by Artemis and NRH.  (a) the Artemis dynamic spectrum; (b-c) total NRH fluxes and (d-e)  polarization levels; (f) the emission spectra at selected moments. The  two vertical lines indicate the flare start and peak time.

 

We further examine the spatial correlation of the radio burst and the  eruptive structure. The radio sources co-move outward with the HC  structure, indicates that the t-IV emitting energetic electrons are  efficiently trapped within this HC structure (see Figure 3). The t-IV  sources at different frequencies present no considerable spatial  dispersion during the early stage of the event (top panels), while the  sources spread gradually along the eruptive HC structure at later stage  with significant spatial dispersion (middle panels).  Later, the sources line up from high to low frequencies (bottom panels).

 

These observations indicate that the t-IVm sources are emitted by energetic  electrons that are first trapped within the plasmoid structure and then  get scattered along the expanding side-arcade structure of the eruptive  HC.


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Fig. 3 - (a-c) Temporal evolution of the NRH sources, superposed onto the  closest-in time AIA 131 Å images. The NRH data are represented by the  95% TBmax contours. The yellow dotted lines present the outline of the side arcade inferred at 10:40 UT.

 

This study demonstrates the possibility of imaging the eruptive HC structure at the metric wavelength and provides strong constraints on the type-IV emitting mechanism, which if understood, can be used to diagnose the  essential parameters of the eruptive structure.

 

The manuscript has been accepted for publication in Astrophysical Journal Letters.

 Please see the manuscript for further details.

(http://arxiv.org/pdf/1609.06546v1.pdf)

 



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