Abstract
New solar type III burst observations are analysed at frequencies between 70-30 MHz. Combining imaging and spectra from LOFAR the apparent velocity of the type III exciter is estimated without the assumption of a density model. The observations suggest that the type IIIs are emitted by an electron beams travelling at relativistic velocities, much faster than predicted from typical coronal models. The type III centroids indicate the electron beams travels along an over-dense solar coronal density structure originating from a solar active region. Assumptions that are normally used to deduce exciter velocities are discussed.
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