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Hot channel (HC) structure, observed in the high-temperature passbands of theAIA/SDO, is regarded as one candidate of coronal flux rope which is anessential element of solar eruptions. Here we present the first radio imagingstudy of an HC structure in the metric wavelength. The associated radioemission manifests as a moving type-IV (t-IVm) burst. We show that the radiosources co-move outwards with the HC, indicating that the t-IV emittingenergetic electrons are efficiently trapped within the structure. The t-IVsources at different frequencies present no considerable spatial dispersionduring the early stage of the event, while the sources spread gradually alongthe eruptive HC structure at later stage with significant spatial dispersion.The t-IV bursts are characterized by a relatively-high brightness temperature($\sim$ 10$^{7}$ $-$ 10$^{9}$ K), a moderate polarization, and a spectral shapethat evolves considerably with time. This study demonstrates the possibility ofimaging the eruptive HC structure at the metric wavelength and provides strongconstraints on the t-IV emision mechanism, which, if understood, can be used todiagnose the essential parameters of the eruptive structure.

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