Abstract
Quasi-periodic pulsations (QPP) of the microwave emission of a solar flare on 2002 July 3, observed with the Nobeyama Radioheliograph (Japan), were investigated with emphasise on the spatial structure of the emission source. It was shown that the time profiles of the variation of the distance between two main sources of the emission and the microwave flux are similar, with a common quasi-periodicity. The most significant QPP is found to be at 30 s. The increase in the microwave emission flux from the Northern source, as well as the increase in the spatiallyintegrated signal, is accompanied by a decrease in the distance between the sources. In contrast, the decrease in the flux corresponds to the decrease in the source separation. This behaviour, together with the observed spatial localisation of the QPP, is very consistent with the vertically polarised global kink mode of the flaring loop.
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