  We present a high fidelity snapshot spectroscopic radio imaging study of a
weak type I solar noise storm which took place during an otherwise
exceptionally quiet time. Using high fidelity images from the Murchison
Widefield Array, we track the observed morphology of the burst source for 70
minutes and identify multiple instances where its integrated flux density and
area are strongly anti-correlated with each other. The type I radio emission is
believed to arise due to electron beams energized during magnetic reconnection
activity. The observed anti-correlation is interpreted as evidence for presence
of MHD sausage wave modes in the magnetic loops and strands along which these
electron beams are propagating. Our observations suggest that the sites of
these small scale reconnections are distributed along the magnetic flux tube.
We hypothesise that small scale reconnections produces electron beams which
quickly get collisionally damped. Hence, the plasma emission produced by them
span only a narrow bandwidth and the features seen even a few MHz apart must
arise from independent electron beams.
