Panel a: mock Stokes V dynamic spectrum of a radio burst due to plasma emission modelled using the Parker Solar wind model with solar parameters, assuming a shock speed of 1000 km s⁻¹ and a S/N of 30. Panel b: frequency-integrated burst brightness as a function of the drift delay and time, modelled using the Parker Solar wind model with solar parameters, assuming a shock speed of 1000 km s⁻¹. The defining ‘bow-tie’-shaped feature of a broadband swept astrophysical signal is clearly visible. The red cross indicates the brightest pixel and its corresponding burst drift.