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Context. Solar radio bursts originate mainly from high energy electronsaccelerated in solar eruptions like solar flares, jets, and coronal massejections. A subcategory of solar radio bursts with short time duration may beused as a proxy to understand the wave generation and propagation within thecorona. Aims. Complete case studies of the source size, position and kinematicsof short term bursts are very rare due to instrumental limitations. Acomprehensive multi-frequency spectroscopic and imaging study was carried outof a clear example of a solar type IIIb-III pair. Methods. In this work, thesource of the radio burst was imaged with the interferometric mode, using theremote baselines of the LOw Frequency ARray (LOFAR). A detailed analysis of thefine structures in the spectrum and of the radio source motion with imaging wasconducted. Results. The study shows how the fundamental and harmonic componentshave a significantly different source motion. The apparent source of thefundamental emission at 26.56MHz displaces away from the solar disk center atabout 4 times the speed of light, while the apparent source of the harmonicemission at the same frequency shows a speed of < 0.02c. The source size of theharmonic emission, observed in this case, is smaller than that in previousstudies, indicating the importance of the use of the remote baselines.

Interferometric Imaging with LOFAR Remote Baselines of the Fine Structures of a Solar Type IIIb Radio Burst